FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Yoo, J AF Yoo, Jaiyul TI General relativistic description of the observed galaxy power spectrum: Do we understand what we measure? SO PHYSICAL REVIEW D LA English DT Article ID DIGITAL SKY SURVEY; PRIMORDIAL NON-GAUSSIANITY; HALO BIAS; PERTURBATIONS AB We extend the general relativistic description of galaxy clustering developed in Yoo, Fitzpatrick, and Zaldarriaga (2009). For the first time we provide a fully general relativistic description of the observed matter power spectrum and the observed galaxy power spectrum with the linear bias ansatz. It is significantly different from the standard Newtonian description on large scales and especially its measurements on large scales can be misinterpreted as the detection of the primordial non-Gaussianity even in the absence thereof. The key difference in the observed galaxy power spectrum arises from the real-space matter fluctuation defined as the matter fluctuation at the hypersurface of the observed redshift. As opposed to the standard description, the shape of the observed galaxy power spectrum evolves in redshift, providing additional cosmological information. While the systematic errors in the standard Newtonian description are negligible in the current galaxy surveys at low redshift, correct general relativistic description is essential for understanding the galaxy power spectrum measurements on large scales in future surveys with redshift depth z >= 3. We discuss ways to improve the detection significance in the current galaxy surveys and comment on applications of our general relativistic formalism in future surveys. C1 Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Yoo, J (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jyoo@cfa.harvard.edu FU Harvard College Observatory FX J. Y. acknowledges useful discussions with Daniel Eisenstein, Eiichiro Komatsu, Uros. Seljak, and Michael Turner. Especially, J. Y. thanks Matias Zaldarriaga for his encouragement and critical comments throughout the completion of this work. J. Y. is supported by the Harvard College Observatory under the Donald H. Menzel fund. NR 32 TC 88 Z9 88 U1 1 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD OCT 7 PY 2010 VL 82 IS 8 AR 083508 DI 10.1103/PhysRevD.82.083508 PG 12 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 660KB UT WOS:000282639300004 ER PT J AU Huang, YM Mathis, WN Wilkerson, RC AF Huang, Yiau-Min Mathis, Wayne N. Wilkerson, Richard C. TI Coetzeemyia, a new subgenus of Aedes, and a redescription of the holotype female of Aedes (Coetzeemyia) fryeri (Theobald) (Diptera: Culicidae) SO ZOOTAXA LA English DT Article DE Coetzeemyia; new subgenus; Aedes fryeri; Ae. dufouri; Ochlerotatus; Levua; Ae. (Levua) geoskusea (=suvae); characteristics; systematics; Culicidae; Aldabra Island ID ALLIED TAXA DIPTERA; LIFE STAGES; MORPHOLOGICAL DATA; AEDINI DIPTERA; CLASSIFICATION; PHYLOGENY; OCHLEROTATUS AB Coetzeemyia, a new subgenus of Aedes Meigen (in the broad traditional sense, pre-Reinert 2000), is characterized and diagnosed. Aedes fryeri (Theobald) is removed from the subgenus Levua Stone and Bohart (genus Levua of Reinert et al. 2004) and placed in the new monotypic subgenus Coetzeemyia as its type species by present designation. Recognition of Coetzeemyia is based in part on a cladistic analysis of 16 species: seven outgroup species (four non-Aedini species and 3 aedine species) and nine within group species, including the three species that had been included in Levua and six other species belonging to three related subgenera in Aedes (Geoskusea Edwards, Rhinoskusea Edwards, and Ochlerotatus-Lynch Arribalzaga). The type female and the male genitalia of Ae. fryeri are redescribed and illustrated. Its affinity to other subgenera of the genus Aedes is discussed. Information on the type data, distribution, bionomics, medical importance, and taxonomy of this species are presented. Some morphological characteristics of adults of the subgenera Ochlerotatus and Levua of Aedes are tabulated. Based on this cladistic analysis, it is evident that Levua is a monotypic lineage represented by a single known species, Ae. geoskusea. Aedes dufouri is transferred back to the subgenus Ochlerotatus and is distinguished from other congeners of this subgenus. C1 [Huang, Yiau-Min; Mathis, Wayne N.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Wilkerson, Richard C.] Smithsonian Inst, WRBU, Washington, DC 20013 USA. [Wilkerson, Richard C.] Walter Reed Army Inst Res, Div Entomol, Silver Spring, MD 20910 USA. RP Huang, YM (reprint author), Smithsonian Inst, Dept Entomol, POB 37012,MSC C1109,MRC 534, Washington, DC 20013 USA. EM huangy@si.edu; mathisw@si.edu; wilkersonr@si.edu FU Department of Entomology, Smithsonian Institution; Walter Reed Army Institute of Research and the Smithsonian Institution FX We express our sincere appreciation and gratitude to the Department of Entomology, Smithsonian Institution for providing funding for the publication; to Drs. Leopoldo M. Rueda and Desmond Foley, Walter Reed Biosystematics Unit (WRBU), for critically reviewing this manuscript, and for their valuable comments. We also thank Ms. Karolyn Darrow, Scientific Illustrator, Department of Entomology, Smithsonian Institution, who helped produce the cladogram (Fig. 4).; This research was performed under a Memorandum of Understanding between the Walter Reed Army Institute of Research and the Smithsonian Institution, with institutional support provided by both organizations. The material to be published reflects the views of the authors and should not be construed to represent those of the Department of the Army or the Department of Defense. NR 28 TC 4 Z9 4 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD OCT 6 PY 2010 IS 2638 BP 1 EP 24 PG 24 WC Zoology SC Zoology GA 660LV UT WOS:000282645300001 ER PT J AU Hohensee, MA Stanwix, PL Tobar, ME Parker, SR Phillips, DF Walsworth, RL AF Hohensee, Michael A. Stanwix, Paul L. Tobar, Michael E. Parker, Stephen R. Phillips, David F. Walsworth, Ronald L. TI Improved constraints on isotropic shift and anisotropies of the speed of light using rotating cryogenic sapphire oscillators SO PHYSICAL REVIEW D LA English DT Article ID ATOMIC CLOCK; TIME AB We demonstrate that Michelson-Morley tests, which detect direction-dependent anisotropies in the speed of light, can also be used to place limits upon isotropic deviations of the vacuum speed of light from c, as described by the photon-sector standard model extension parameter (kappa) over tilde (tr). A shift in the speed of light that is isotropic in one inertial frame implies anisotropic shifts in others. Using observer Lorentz covariance, we derive the time-dependent variations in the relative resonance frequencies of a pair of electromagnetic resonators that would be generated by such a shift in the rest frame of the Sun. A new analysis of a recent experimental test of relativity using this result constrains (kappa) over tilde (tr) with a precision of 7.4 x 10(-9). This represents the first constraint on (kappa) over tilde (tr) by a Michelson-Morley experiment and the first analysis of a single experiment to simultaneously set limits on all nine nonbirefringent terms in the photon sector of the minimal standard model extension. C1 [Hohensee, Michael A.; Walsworth, Ronald L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Hohensee, Michael A.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Stanwix, Paul L.; Tobar, Michael E.; Parker, Stephen R.] Univ Western Australia, Sch Phys, Nedlands, WA 6009, Australia. [Stanwix, Paul L.; Phillips, David F.; Walsworth, Ronald L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Hohensee, MA (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. EM hohensee@berkeley.edu RI Stanwix, Paul/A-5280-2009; Parker, Stephen/I-4231-2013; Tobar, Michael/C-9763-2009; OI Stanwix, Paul/0000-0002-7069-8569; Parker, Stephen/0000-0003-1914-8833; Tobar, Michael/0000-0002-3139-1994; Hohensee, Michael/0000-0002-8106-4502 FU National Science Foundation; Australian Research Council FX This work was supported by the National Science Foundation and the Australian Research Council. We thank Alan Kostelecky and Ralf Lehnert for encouragement and useful discussions. NR 29 TC 18 Z9 18 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD OCT 5 PY 2010 VL 82 IS 7 AR 076001 DI 10.1103/PhysRevD.82.076001 PG 9 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 658SG UT WOS:000282509100006 ER PT J AU Case, AW Spence, HE Golightly, MJ Kasper, JC Blake, JB Mazur, JE Townsend, LW Zeitlin, CJ AF Case, A. W. Spence, H. E. Golightly, M. J. Kasper, J. C. Blake, J. B. Mazur, J. E. Townsend, L. W. Zeitlin, C. J. TI GCR access to the Moon as measured by the CRaTER instrument on LRO SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ADVANCED COMPOSITION EXPLORER; SOLAR-WIND; MAGNETOPAUSE; PARTICLES AB Recent modeling efforts have yielded varying and conflicting results regarding the possibility that Earth's magnetosphere is able to shield energetic particles of >10 MeV at lunar distances. This population of particles consists of galactic cosmic rays as well as energetic particles that are accelerated by solar flares and coronal mass ejections. The Cosmic Ray Telescope for the Effects of Radiation (CRaTER) onboard the Lunar Reconnaissance Orbiter is in orbit about the Moon and is thus able to directly test these modeling results. Over the course of a month, CRaTER samples the upstream solar wind as well as various regions of Earth's magnetotail. CRaTER data from multiple lunations demonstrate that Earth's magnetosphere at lunar distances produces no measurable influence on energetic particle flux, even at the lowest energies (>14 MeV protons) where any effect should be maximized. For particles with energies of 14-30 MeV, we calculate an upper limit (determined by counting statistics) on the amount of shielding caused by the magnetosphere of 1.7%. The high energy channel (>500 MeV) provides an upper limit of 3.2%. Citation: Case, A. W., H. E. Spence, M. J. Golightly, J. C. Kasper, J. B. Blake, J. E. Mazur, L. W. Townsend, and C. J. Zeitlin (2010), GCR access to the Moon as measured by the CRaTER instrument on LRO, Geophys. Res. Lett., 37, L19101, doi: 10.1029/2010GL045118. C1 [Case, A. W.] Boston Univ, Ctr Space Phys, Boston, MA 02215 USA. [Blake, J. B.] Aerosp Corp, El Segundo, CA 90245 USA. [Spence, H. E.; Golightly, M. J.] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA. [Kasper, J. C.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Mazur, J. E.] Aerosp Corp, Conf Ctr, Chantilly, VA 20151 USA. [Townsend, L. W.] Univ Tennessee, Dept Nucl Engn, Knoxville, TN 37996 USA. [Zeitlin, C. J.] SW Res Inst, Boulder, CO 80302 USA. RP Case, AW (reprint author), Boston Univ, Ctr Space Phys, 725 Commonwealth Ave, Boston, MA 02215 USA. EM tonycase@bu.edu RI Kasper, Justin/D-1152-2010; Spence, Harlan/A-1942-2011 OI Spence, Harlan/0000-0002-2526-2205; Kasper, Justin/0000-0002-7077-930X; FU LRO/CRaTER [NASA NNG05EB92C] FX We would like to thank Chia-Lin Huang for helpful discussions, Dick Mewaldt and the SIS instrument team for providing GCR data from the ACE spacecraft, and the ACE SWEPAM team and the ACE Science Center for providing the ACE solar wind data. This work was supported by the LRO/CRaTER project under contract NASA NNG05EB92C. NR 14 TC 2 Z9 3 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD OCT 2 PY 2010 VL 37 AR L19101 DI 10.1029/2010GL045118 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 657SQ UT WOS:000282433000009 ER PT J AU Harbaugh, DT Oppenheimer, HL Wood, KR Wagner, WL AF Harbaugh, Danica T. Oppenheimer, Hank L. Wood, Kenneth R. Wagner, Warren L. TI Taxonomic Revision of the Endangered Hawaiian Red-flowered Sandalwoods (Santalum) and Discovery of an Ancient Hybrid Species SO SYSTEMATIC BOTANY LA English DT Article DE endangered species; Hawaiian Islands; microsatellites; molecular phylogeny; morphology; taxonomic revision ID SILVERSWORD ALLIANCE COMPOSITAE; SANTALACEAE; PACIFIC; KAUAI; INSULARE; CONSERVATION; ISLANDS; NUCLEAR; GENUS AB The Hawaiian Islands are home to a quarter of the named diversity of sandalwoods in the genus Santa him. There has been considerable confusion on how to best interpret the variation patterns of the red-flowered Hawaiian sandalwoods, S.freycinetianum and S. haleakalae, and particularly of the endangered S. freycinetianum var. lanaiense in an appropriate taxonomy. In this study, nrDNA (ITS, ETS) and cpDNA (3' trnK intron) sequence, microsatellite, and morphological data are integrated to appropriately revise the taxonomy of this group by better understanding the genetic and morphological diversity within and between populations. Results reveal that populations of S. freycinetianum from O'ahu are genetically distinct from populations on Moloka'i, Lana'i, and Maui. Santalum freycinatianum is now considered only to occur on O'ahu. The East Maui endemic S. haleakalae intergrades morphologically and is not genetically distinct from populations of S. freycinetianum var. lanaiense based on the sequence and microsatellite data gathered thus far. We combine them here into a single species, S. haleakalae, with two varieties (var. haleakalae and var. lanaiense, comb nov.). Lastly, examination of populations of S. freycinetianum var. pyrularium suggest it is best treated at specific rank as S. pyrularium. Some populations that are sympatric with S. pyrularium and S. ellipticum in the coastal cliffs and valleys of northern Kaua'i, are morphologically similar to S. pyrularium but are more closely related to the white-flowered S. ellipticum clade according to both nrDNA and cpDNA data. However, at least three synapomorphic sites in the nrDNA data indicate that its origin may have been the result of an ancient hybridization event with the red-flowered clade. The morphological characteristics of this inferred ancient hybrid lineage appear to correspond with the species S. involutum described by H. St. John. C1 [Harbaugh, Danica T.; Wagner, Warren L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Oppenheimer, Hank L.] Univ Hawaii, Plant Extinct Prevent Program, Pacific Cooperat Studies Unit, Lahaina, HI 96761 USA. [Wood, Kenneth R.] Natl Trop Bot Garden, Kauai, HI 96741 USA. RP Harbaugh, DT (reprint author), Univ Calif Berkeley, 1001 Valley Life Sci Bldg 2465, Berkeley, CA 94720 USA. EM danicah@berkeley.edu FU National Tropical Botanical Garden on Kauai; Department of Botany; National Museum of Natural History; Smithsonian Institution FX The authors thank the associate editor of Systematic Botany, M. Wojciechowski, B. Baldwin, an anonymous reviewer, and D. Lorence for their invaluable comments and suggestions for improvement of the manuscript, as well as the numerous organizations and people who made this research possible by providing herbarium material to examine, permission to collect material in the field, or assistance in collecting it, including: The Bishop Museum (A. Harbottle); The National Tropical Botanical Garden (T. Flynn, D. Lorence, and C. Wichman); The Nature Conservancy, Molokai field office (E. Misaki and K Tachibana); East Molokai Watershed Partnership; Castle & Cooke (B. Plunkett); Maui Land & Pineapple Co. Pu'u Kukui Watershed Preserve (R. Bartlett and M. Webster); West Maui Mountains Watershed Partnership; Makila Land Co.; Leeward Haleakala Watershed Restoration Partnership; Hawai'i Division of Forestry & Wildlife; Kauai State Parks; Haleakala Ranch (S. Meidell), Haleakala National Park (E. Gordon, P. Welton, S. Anderson); Army Natural Resources, O'ahu (S. Ching and K. Welch, N. Maileau, J. Rohrer, M. Keir); The Nature Conservancy, Honouliuli Preserve field office (S. Lu, D. Sailer, D. Forman, L. Williams, M. Walker and J. Chu); The Nature Conservancy Maui office (P. Bily); The Nature Conservancy, Kanepu'u Preserve (R. Hera, R. Sabin, M. Eskaren, A. Amoncio, Ike Aina); Ulupalakua Ranch Auwahi Preserve (A. Medeiros, K. Bustamente, and F. Juan), A. Smith and B. Baldwin (UC Berkeley); R. Hobdy (DOFAW, ret.); U. S. Fish and Wildlife Service; S. Perlman (National Tropical Botanical Garden); and D. Reynaud. The authors also thank B. Baldwin and B. Wessa for assistance with molecular phylogenetic work at the Molecular Phylogenetics Laboratory at the University of California, Berkeley, as well as R. Fleischer and N. Rotzel for their assistance with microsatellite genotyping at the Center for Conservation and Evolutionary Genetics at the Smithsonian National Zoological Park, Washington, DC. Lastly, they thank the National Tropical Botanical Garden on Kauai (McBryde Science Program) and the Department of Botany, National Museum of Natural History, Smithsonian Institution for funding to D. Harbaugh for field and laboratory expenses, while appointed as a McBryde Postdoctoral Research Fellow. NR 48 TC 4 Z9 5 U1 6 U2 15 PU AMER SOC PLANT TAXONOMISTS PI LARAMIE PA UNIV WYOMING, DEPT BOTANY 3165, 1000 E UNIVERSITY AVE, LARAMIE, WY 82071 USA SN 0363-6445 J9 SYST BOT JI Syst. Bot. PD OCT-DEC PY 2010 VL 35 IS 4 BP 827 EP 838 DI 10.1600/036364410X539899 PG 12 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 693JV UT WOS:000285221300013 ER PT J AU Flacke, G Spiering, P Cooper, D Gunther, MS Robertson, I Palmer, C Warren, K AF Flacke, Gabriella Spiering, Penny Cooper, Dave Gunther, Micaela Szykman Robertson, Ian Palmer, Carlysle Warren, Kristin TI A survey of internal parasites in free-ranging African wild dogs (Lycaon pictus) from KwaZulu-Natal, South Africa SO SOUTH AFRICAN JOURNAL OF WILDLIFE RESEARCH LA English DT Article DE Ancylostoma; Babesia canis; Dipylidium caninum; Ehrlichia canis; internal parasites; Isospora; Sarcocystis; Toxocara canis ID CANIS-MESOMELAS SCHREBER; TRANSMISSION; TEMMINCK AB A study was undertaken between 1 January 2006 and 16 February 2007 to identify haemoparasites and gastrointestinal parasites infecting African wild dogs (Lycaon pictus) in KwaZulu-Natal (KZN) province, South Africa. Blood and faecal samples were opportunistically collected from wild dogs immobilized for collaring or translocation purposes (n = 24). Three common domestic canine gastrointestinal parasites, Toxocara canis, Dipylidium caninum and Ancylostoma spp., and two genera of canid protozoan GI parasites, Sarcocystis and Isospora, were identified in 12 fresh faecal samples. The seroprevalence of Ehrlichia canis from 24 individual serum samples analysed was 83%. However, only 21% of the 14 whole-blood smears evaluated for the presence of E. canis morulae within monocytes were positive. Twelve whole-blood smears were evaluated for the presence of Babesia canistrophozoites within erythrocytes and revealed 0% prevalence. Although there is currently no evidence of direct parasite-related mortality in the KZN population, the presence of internal parasites may be more detrimental to the overall health status of African wild dogs with immunosuppression as a result of other disease conditions, translocation stress, or inbreeding depression. C1 [Flacke, Gabriella; Palmer, Carlysle; Warren, Kristin] Murdoch Univ, Sch Vet & Biomed Sci, Conservat Med Programme, Perth, WA 6150, Australia. [Spiering, Penny; Gunther, Micaela Szykman] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA. [Spiering, Penny] Univ Pretoria, Ctr Wildlife Management, ZA-0002 Pretoria, South Africa. [Cooper, Dave] Ezemvelo KZN Wildlife, ZA-3202 Pietermaritzburg, South Africa. [Gunther, Micaela Szykman] Humboldt State Univ, Dept Wildlife, Arcata, CA 95521 USA. [Robertson, Ian] Murdoch Univ, Sch Vet & Biomed Sci, Vet Epidemiol Programme, Perth, WA 6150, Australia. RP Flacke, G (reprint author), Murdoch Univ, Sch Vet & Biomed Sci, Conservat Med Programme, Perth, WA 6150, Australia. EM gflacke@hotmail.com FU National Geographic Society Conservation Trust [C91-06]; Murdoch University FX We thank the management of Hluhluwe-iMfolozi Park, the Isimangaliso (Greater St Lucia) Wetland Park Authority, Mkhuze Game Reserve and Thanda Private Game Reserve for permission to conduct this research and for logistical support. We also thank the Ezemvelo-KZN Wildlife Game Capture Unit for use of darting and laboratory equipment. Furthermore, we thank Moritz van Vuuren and the laboratory at the Department of Veterinary Tropical Diseases, Onderstepoort, for conducting the serology for this project, and Darryl Baxter, Heinz Kohrs and Trevor Viljoen, private practice veterinarians who contributed information on disease prevalence in domestic dogs in KZN. Finally, we wish to thank Sboniso Zwane and Thadaigh Baggallay for assistance with field monitoring. This project was supported by the National Geographic Society Conservation Trust (Grant Number C91-06) and the Conservation Medicine Small Research Grants Programme at Murdoch University. NR 19 TC 3 Z9 3 U1 1 U2 10 PU SOUTHERN AFRICAN WILDLIFE MANAGEMENT ASSOC PI BLOUBERGSTRAND PA P O BOX 217, BLOUBERGSTRAND 7437, SOUTH AFRICA SN 0379-4369 J9 S AFR J WILDL RES JI South Afr. J. Wildl. Res. PD OCT PY 2010 VL 40 IS 2 BP 176 EP 180 PG 5 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA 769KO UT WOS:000291012100010 ER PT J AU D'Apolito, C Pessoa, SM Balestieri, FCDM Balestieri, JBP AF D'Apolito, Carlos Pessoa, Sheila Magalhaes de Lazari Manente Balestieri, Fatima Cristina Perrella Balestieri, Jose Benedito TI Pollen harvest by Apis mellifera L. (Hymenoptera: Apidae) in the Dourados region, Mato Grosso do Sul state (Brazil) SO ACTA BOTANICA BRASILICA LA English DT Article DE bee flora; Brazilian center west ID AFRICANIZED HONEY-BEE; ATLANTIC RAIN-FOREST; STINGLESS BEES; MELIPONA; APOIDEA AB (Pollen harvest by Apis mellifera L. (Hymenoptera: Apidae) in the Dourados region, Mato Grosso do Sul state (Brazil)). We present data on the pollen harvest by Apis mellifera L. at a central-western Brazil site not yet studied. Corbiculae pollen loads were collected during one year in front of the hive, acetolysed and slides mounted for optical microscopy. Identification followed comparisons with a local pollen collection. Forty-two pollen types were utilized by the bee; the most important families were Myrtaceae, Asteraceae, Euphorbiaceae, Brassicaceae and Poaceae. The genus/species level ranking of relative importance showed Eucalyptus (19%), Raphanus raphanistrum (13%), Poaceae type 2 (7.5%), Jatropha cf. gossypiifolia (7%) and Sapium glandulatum (6.5%). Overall, the majority of pollen types (80%) were not abundantly harvested, and a minority (4%) reached values of 10%. Given that the study area has cultivated plants and not natural vegetation, we indicate most of the identified species as manageable and point out that weedy vegetation can be an important food source for bees since it frequently occurred in the pollen spectra even within a totally cultivated area. C1 [D'Apolito, Carlos] Ancon, Smithsonian Trop Res Inst, Panama City, Panama. [Pessoa, Sheila Magalhaes] Fundacao Univ Fed Grande Dourados, Fac Ciencias Agr, Dourados, MS, Brazil. [de Lazari Manente Balestieri, Fatima Cristina; Perrella Balestieri, Jose Benedito] Fundacao Univ Fed Grande Dourados, Fac Ciencias Biol & Ambientais, Lab Abelhas Nativas, Dourados, MS, Brazil. RP D'Apolito, C (reprint author), Ancon, Smithsonian Trop Res Inst, Panama City, Panama. EM carlosdapolito@hotmail.com NR 37 TC 1 Z9 1 U1 1 U2 5 PU SOC BOTANICA BRASIL PI SAO PAULO SP PA CAIXA POSTAL 3005, SAO PAULO SP, 01061-970, BRAZIL SN 0102-3306 EI 1677-941X J9 ACTA BOT BRAS JI Acta Bot. Bras. PD OCT-DEC PY 2010 VL 24 IS 4 BP 898 EP 904 PG 7 WC Plant Sciences SC Plant Sciences GA 728RB UT WOS:000287891100003 ER PT J AU Lee, CF Staines, CL AF Lee, Chi-Feng Staines, Charles L. TI MONOLEPTA ONGI, A NEW SPECIES FROM LANYU ISLAND, WITH REDESCRIPTION OF ITS ALLIED SPECIES MONOLEPTA LONGITARSOIDES CHUJO, 1938 (COLEOPTERA: CHRYSOMELIDAE: GALERUCINAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE color variation; Taiwan; taxonomy ID REVISION AB Monolepta ongi, n. sp., is described from Lanyu Island, Taitung county, Taiwan. Its allied species, Monolepta longitarsoides Chujo, 1938, is redescribed for comparison. Their antennae, male aedeagus, female spermatheca and bursa-sclerites are illustrated. The lectotype and paralectotypes are designated for Monolepta longitarsoides from Chujo's type series. C1 [Lee, Chi-Feng] Agr Res Inst Taiwan, Appl Zool Div, Taichung 413, Wufeng, Taiwan. [Staines, Charles L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, MRC 187, Washington, DC 20013 USA. RP Lee, CF (reprint author), Agr Res Inst Taiwan, Appl Zool Div, 189 Chung Cheng Rd, Taichung 413, Wufeng, Taiwan. EM chifeng@tari.gov.tw; stainesc@si.edu NR 20 TC 0 Z9 0 U1 1 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2010 VL 112 IS 4 BP 530 EP 540 DI 10.4289/0013-8797.112.4.530 PG 11 WC Entomology SC Entomology GA 708IN UT WOS:000286355600007 ER PT J AU Walters, JR Derrickson, SR Fry, DM Haig, SM Marzluff, JM Wunderle, JM AF Walters, Jeffrey R. Derrickson, Scott R. Fry, D. Michael Haig, Susan M. Marzluff, John M. Wunderle, Joseph M., Jr. TI STATUS OF THE CALIFORNIA CONDOR (GYMNOGYPS CALIFORNIANUS) AND EFFORTS TO ACHIEVE ITS RECOVERY SO AUK LA English DT Editorial Material ID ENDANGERED-SPECIES-ACT; ENVIRONMENTAL CONTAMINANTS; LEAD; CONSERVATION; POPULATION; MANAGEMENT; AMMUNITION; VULTURES; REINTRODUCTION; REPRODUCTION C1 [Walters, Jeffrey R.] Virginia Tech Univ, Dept Biol Sci, Blacksburg, VA 24061 USA. [Derrickson, Scott R.] Smithsonian Conservat Res Ctr, Front Royal, VA 22630 USA. [Fry, D. Michael] Amer Bird Conservancy, Washington, DC 20009 USA. [Haig, Susan M.] Oregon State Univ, US Geol Survey, Forest & Rangeland Ecosyst Sci Ctr, Corvallis, OR 97331 USA. [Marzluff, John M.] Univ Washington, Coll Environm, Seattle, WA 98195 USA. [Wunderle, Joseph M., Jr.] Int Inst Trop Forestry, USDA, Forest Serv, Sabana Field Res Stn, Luquillo, PR 00773 USA. RP Walters, JR (reprint author), Virginia Tech Univ, Dept Biol Sci, Blacksburg, VA 24061 USA. EM jrwalt@vt.edu NR 109 TC 41 Z9 43 U1 14 U2 117 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 J9 AUK JI AUK PD OCT PY 2010 VL 127 IS 4 BP 969 EP 1001 DI 10.1525/auk.2010.127.4.969 PG 33 WC Ornithology SC Zoology GA 679XZ UT WOS:000284195400027 ER PT J AU da Silva-Caminha, SAF Jaramillo, CA Absy, ML AF da Silva-Caminha, Silane A. F. Jaramillo, Carlos A. Absy, Maria Lucia TI Neogene palynology of the Solimoes Basin, Brazilian Amazonia SO PALAEONTOGRAPHICA ABTEILUNG B-PALAEOPHYTOLOGIE PALAEOBOTANY-PALAEOPHYTOLOGY LA English DT Article DE Palynology; taxonomy; stratigraphy; Neogene; Amazonia ID LATE-MIOCENE; QUANTITATIVE BIOCHRONOLOGY; TERTIARY SEDIMENTS; RECONSTRUCTION; CONSERVATION; COLOMBIA; POLLEN; SPORES; AGE AB The tropics of South America hold the largest plant diversity in the world, yet the origins and processes leading to this high diversity still remain elusive. The Neogene sedimentary and fossil record of Amazonia could contain important clues to understanding the evolution of the Amazonian forest. Here, we study the pollen and spore record of two drill cores of the Neogene Solimoes Formation taken in northwestern Brazil, east of the Iquitos Arch. We studied 41 palynological samples and used several techniques to analyze the results, including Unitary Associations, a quantitative biostratigraphic technique, and Multidimensional Scaling Analysis. We describe 109 species, 51 of which are new, and seven new combinations. The biostratigraphic analysis indicates that the age of the Solimoes Formation in the study area is Late Miocene/Early Pliocene. This age is younger than that of nearby sections located west of the Iquitos arch, suggesting that the Iquitos Arch was active during the accumulation of the Solimoes Formation. The pollen/spore assemblages indicate that the Solimoes accumulated in fluvial deposits. We did not find evidence of either marine/tidal-flat deposits or extensive lakes. C1 [da Silva-Caminha, Silane A. F.; Absy, Maria Lucia] Lab Palinol CPBO INPA, Cordenacao Pos Grad Ecol PGEC, INPA, BR-69011970 Manaus, Amazonas, Brazil. [da Silva-Caminha, Silane A. F.; Jaramillo, Carlos A.] Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama. RP da Silva-Caminha, SAF (reprint author), Lab Palinol CPBO INPA, Cordenacao Pos Grad Ecol PGEC, INPA, POB 478, BR-69011970 Manaus, Amazonas, Brazil. FU CAPES; CNPq FX We thank the Smithsonian Tropical Research Institute (STRI) and Instituto Nacional de Pesquisas da Amazonia (INPA) where this research was carried out. We also thank Departamento Nacional de Prospeccao Mineral (DNPM), especially Dr. Fernando Burgos and Gert Woeltje for the sampling permits of the Amazon cores. We thank Instituto Colombiano del Petroleo (ICP) for sample processing. Thanks to Dr. Jean Guex for the biostratigraphical comments; Dr. Jackson Paz, Dr. Fatima Leite, Dr. Edgardo Latrubesse for the geological discussions; Millerlandy Romero, Paula Sucerquia and Jean Caminha for help with the figures; Giovanni Bedoya for the corrections in the Latin names; and especially, Milton Rueda for the palynological morphology discussions. Thanks to Dr. Carmen Schloeder and Dr. Florian Wittmann for the translation of the abstract into German. Thanks to A. Traverse, D. Dilcher, T. Lott and D. Mai for their helpful comments on the manuscript. This study was supported by CAPES and CNPq Brazilian fellowships. NR 114 TC 3 Z9 3 U1 0 U2 5 PU E SCHWEIZERBARTSCHE VERLAGSBUCHHANDLUNG PI STUTTGART PA NAEGELE U OBERMILLER, SCIENCE PUBLISHERS, JOHANNESSTRASSE 3A, D 70176 STUTTGART, GERMANY SN 0375-0299 J9 PALAEONTOGR ABT B JI Palaeontogr. Abt. B-Palaophytol. PD OCT PY 2010 VL 284 IS 1-3 BP 13 EP 79 PG 67 WC Paleontology SC Paleontology GA 679XE UT WOS:000284193300002 ER PT J AU LaFollette, MC AF LaFollette, Marcel Chotkowski TI Keep Watching the Skies! The Story of Operation Moonwatch and the Dawn of the Space Age SO AMERICAN HISTORICAL REVIEW LA English DT Book Review C1 [LaFollette, Marcel Chotkowski] Smithsonian Inst, Washington, DC 20560 USA. RP LaFollette, MC (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0002-8762 J9 AM HIST REV JI Am. Hist. Rev. PD OCT PY 2010 VL 115 IS 4 BP 1177 EP 1177 PG 1 WC History SC History GA 669ZB UT WOS:000283387800089 ER PT J AU Turner, BL AF Turner, Benjamin L. TI Variation in pH Optima of Hydrolytic Enzyme Activities in Tropical Rain Forest Soils SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID MICROBIAL COMMUNITY COMPOSITION; PHOSPHATASE-ACTIVITY; CELLULASE-ACTIVITY; CHITINASE ACTIVITY; BETA-GLUCOSIDASE; ACID-PHOSPHATASE; WETLAND SOILS; PHOSPHODIESTERASE; LITTER; ASSAY AB Extracellular enzymes synthesized by soil microbes play a central role in the biogeochemical cycling of nutrients in the environment. The pH optima of eight hydrolytic enzymes involved in the cycles of carbon, nitrogen, phosphorus, and sulfur, were assessed in a series of tropical forest soils of contrasting pH values from the Republic of Panama. Assays were conducted using 4-methylumbelliferone-linked fluorogenic substrates in modified universal buffer. Optimum pH values differed markedly among enzymes and soils. Enzymes were grouped into three classes based on their pH optima: (i) enzymes with acidic pH optima that were consistent among soils (cellobiohydrolase, beta-xylanase, and arylsulfatase), (ii) enzymes with acidic pH optima that varied systematically with soil pH, with the most acidic pH optima in the most acidic soils (alpha-glucosidase, beta-glucosidase, and N-acetyl-beta-glucosaminidase), and (iii) enzymes with an optimum pH in either the acid range or the alkaline range depending on soil pH (phosphomonoesterase and phosphodiesterase). The optimum pH values of phosphomonoesterase were consistent among soils, being 4 to 5 for acid phosphomonoesterase and 10 to 11 for alkaline phosphomonoesterase. In contrast, the optimum pH for phosphodiesterase activity varied systematically with soil pH, with the most acidic pH optima (3.0) in the most acidic soils and the most alkaline pH optima (pH 10) in near-neutral soils. Arylsulfatase activity had a very acidic optimum pH in all soils (pH <= 3.0) irrespective of soil pH. The differences in pH optima may be linked to the origins of the enzymes and/or the degree of stabilization on solid surfaces. The results have important implications for the interpretation of hydrolytic enzyme assays using fluorogenic substrates. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Turner, BL (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM TurnerBL@si.edu RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 NR 63 TC 49 Z9 54 U1 3 U2 62 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0099-2240 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD OCT PY 2010 VL 76 IS 19 BP 6485 EP 6493 DI 10.1128/AEM.00560-10 PG 9 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 653ZA UT WOS:000282136700019 PM 20709838 ER PT J AU Baldwin, AH Kettenring, KM Whigham, DF AF Baldwin, Andrew H. Kettenring, Karin M. Whigham, Dennis F. TI Seed banks of Phragmites australis-dominated brackish wetlands: Relationships to seed viability, inundation, and land cover SO AQUATIC BOTANY LA English DT Article DE Seed banks; Phragmites australis; Common reed; Non-native haplotype; Tidal wetlands; Chesapeake Bay; Wave disturbance; Seedling recruitment; Seed viability; Genetic diversity ID SALT-MARSH PLANTS; COMMON REED; CHESAPEAKE BAY; NEW-JERSEY; VEGETATION; EXPANSION; EMERGENCE; SALINITY; DRAWDOWN; FLUCTUATIONS AB In tidal wetlands of the eastern United States, buried seeds of the non-native haplotype of Phragmites australis may be a source of propagules for re-establishment after eradication efforts but factors controlling the development and expression of seed banks in non-native Phragmites stands have not been examined. We sampled surface soil at four Chesapeake Bay brackish tidal wetlands dominated by the non-native (European) haplotype M of Phragmites and used the seedling emergence method to quantity species of seedlings emerging under flooded and non-flooded soil conditions. Within each subestuary, one site was dominated by Phragmites that produced viable seeds (high viability) and the other by Phragmites that did not (low viability). We also described standing vegetation in plots, measured soil salinity, analyzed soil characteristics, and described surrounding land cover. Based on number of emerging seedlings, we found that 284 and 698 Phragmites seeds m(-2) occurred at the two high-viability sites, which was significantly higher than seed densities at the low-viability sites (10 seeds m-2), and greater than densities reported elsewhere. We also found that emergence of Phragmites seedlings from soil samples was prevented by continuous flooding of 3.5 cm of standing water, suggesting that colonization of deep water areas is clue to vegetative clonal expansion from Phragmites in adjacent higher elevations. The density of Phragmites seeds was not related to soil salinity or abundance of other species in the seed bank or vegetation, but instead was positively related to greater wave energy disturbance (much longer fetch and more open water) and lower area of wetlands nearby. The seed bank was more species-rich (15-22 species observed) than standing vegetation (3-15 species) at all sites, meaning that the dominance of Phragmites in vegetation does not prevent the development of a diverse seed bank and implying that a species-rich community may establish rapidly following control efforts. Based on these results and our findings in related studies, we postulate that wave energy disturbance generates repeated opportunities for seedling recruitment by Phragmites, which creates stands of Phragmites with higher genotypic diversity. In turn, genetically diverse stands favor greater cross-pollination and production of viable seed. These findings suggest that, in North America, targeting control efforts on non-native Phragmites patches in areas of higher exposure to wave energy may be more effective in reducing source populations than efforts in more protected locations. (C) 2010 Elsevier B.V. All rights reserved. C1 [Baldwin, Andrew H.] Univ Maryland, Dept Environm Sci & Technol, College Pk, MD 20742 USA. [Kettenring, Karin M.; Whigham, Dennis F.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Baldwin, AH (reprint author), Univ Maryland, Dept Environm Sci & Technol, 1423 Anim Sci Bldg, College Pk, MD 20742 USA. EM baldwin@umd.edu; karin.kettenring@usu.edu; whighamd@si.edu RI Baldwin, Andrew/C-8759-2014; OI Whigham, Dennis/0000-0003-1488-820X FU Smithsonian Institution FX We thank Pete Sharpe for help in the field and Rose Johnson and Jennifer Van Renterghen for assistance in the greenhouse. Heather Baron assisted with the GIS analysis and produced the maps in Fig. 1. K.M. Kettenring was supported by a Smithsonian Institution Post-Doctoral Fellowship. NR 39 TC 21 Z9 22 U1 6 U2 38 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-3770 J9 AQUAT BOT JI Aquat. Bot. PD OCT PY 2010 VL 93 IS 3 BP 163 EP 169 DI 10.1016/j.aquabot.2010.06.001 PG 7 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 650UH UT WOS:000281877600004 ER PT J AU Dickinson, EC David, N Overstreet, LK Steinheimer, FD Jansen, J AF Dickinson, Edward C. David, Normand Overstreet, Leslie K. Steinheimer, Frank D. Jansen, Justin TI Histoire naturelle des pigeons or Les pigeons: Coenraad Jacob Temminck versus Pauline Knip SO ARCHIVES OF NATURAL HISTORY LA English DT Article DE Pauline de Courcelles; fine art; wrappers; deceit; Empress Marie Louise Bonaparte; Napoleon Bonaparte AB Evidence for the dates of the parts of C. J. Temminck's Histoire naturelle des pigeons was planted by the artist who, with the benefit of royal patronage, had earlier made herself the apparent architect of the work as a whole and renamed it Les pigeons. We here reveal the flaws in the planted evidence, available in Philadelphia, and how these flaws show when she committed the deed. Wrappers play a major role, and a set in Berlin reveals the true dates of publication. The consequence is that the work must be seen as two works: one, the combined issue of the last parts where the artist must be allowed her pride of place; the other, the bulk of the work where her evidence crumbles and Temminck is undoubtedly and lead player in the publication not just the author. C1 [Overstreet, Leslie K.] Smithsonian Inst Libraries, Washington, DC 20013 USA. [Steinheimer, Frank D.] Nat Kundliches Univ Museum, D-06108 Halle, Saale, Germany. RP Dickinson, EC (reprint author), Flat 3,19 Bolsover Rd, Eastbourne BN20 7JG, England. EM edward@asiaorn.org NR 25 TC 2 Z9 2 U1 0 U2 0 PU EDINBURGH UNIV PRESS PI EDINBURGH PA 22 GEORGE SQUARE, EDINBURGH EH8 9LF, MIDLOTHIAN, SCOTLAND SN 0260-9541 J9 ARCH NAT HIST JI Arch. Nat. Hist. PD OCT PY 2010 VL 37 IS 2 BP 203 EP 220 DI 10.3366/E0260954110001944 PG 18 WC History & Philosophy Of Science; Multidisciplinary Sciences SC History & Philosophy of Science; Science & Technology - Other Topics GA 846JC UT WOS:000296892200002 ER PT J AU Olson, SL AF Olson, Storrs L. TI James Petiver's "Mary-Land Yellow-Throat" - a bird misidentified through four centuries SO ARCHIVES OF NATURAL HISTORY LA English DT Article DE common yellowthroat; Dendroica dominica; George Edwards; Geothlypis trichas; Hugh Jones; Parulidae; yellow-throated warbler AB The name "Mary-Land Yellow-Throat" coined by James Petiver in 1702 was subsequently applied to the bird now known as the common yellowthroat, Geothlypis trichas, and the term "yellowthroat", ultimately derivable from Petiver, is now used as a generic term for all nine species of the warbler genus Geothlypis (Parulidae). Re-examination of Petiver's illustration shows that his bird cannot have been a Geothlypis warbler and was almost certainly the yellow-throated warbler, Dendroica dominica. C1 Smithsonian Inst, Div Birds, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Olson, SL (reprint author), Smithsonian Inst, Div Birds, Dept Vertebrate Zool, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA. EM olsons@si.edu NR 26 TC 0 Z9 0 U1 1 U2 1 PU EDINBURGH UNIV PRESS PI EDINBURGH PA 22 GEORGE SQUARE, EDINBURGH EH8 9LF, MIDLOTHIAN, SCOTLAND SN 0260-9541 J9 ARCH NAT HIST JI Arch. Nat. Hist. PD OCT PY 2010 VL 37 IS 2 BP 221 EP 226 DI 10.3366/E0260954110001956 PG 6 WC History & Philosophy Of Science; Multidisciplinary Sciences SC History & Philosophy of Science; Science & Technology - Other Topics GA 846JC UT WOS:000296892200003 ER PT J AU Dorr, LJ AF Dorr, L. J. TI "Muy poco se sabe de los resultados": Francis E. Bond's expedition to the Paria Peninsula and delta of the Orinoco, Venezuela (1911) SO ARCHIVES OF NATURAL HISTORY LA English DT Article DE James Bond; Stewardson Brown; Thomas S. Gillin; natural history exploration AB The natural history expedition of the American banker and stock broker Francis E. Bond and companions to the Paria Peninsula and delta of the Orinoco. Venezuela, in early 1911 is described. Biographical details are provided for the three principals; Francis E. Bond, Stewardson Brown and Thomas S. Gillin. The itinerary of their three and a half month expedition is elaborated, and notes are provided on the collections of plants, animals, and artefacts that they gathered in South America and deposited in the Academy of Natural Sciences of Philadelphia on their return. C1 Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Dorr, LJ (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC-166,POB 37012, Washington, DC 20013 USA. EM dorrl@si.edu NR 91 TC 1 Z9 1 U1 0 U2 0 PU EDINBURGH UNIV PRESS PI EDINBURGH PA 22 GEORGE SQUARE, EDINBURGH EH8 9LF, MIDLOTHIAN, SCOTLAND SN 0260-9541 J9 ARCH NAT HIST JI Arch. Nat. Hist. PD OCT PY 2010 VL 37 IS 2 BP 292 EP 308 DI 10.3366/E0260954110002019 PG 17 WC History & Philosophy Of Science; Multidisciplinary Sciences SC History & Philosophy of Science; Science & Technology - Other Topics GA 846JC UT WOS:000296892200009 PM 21137585 ER PT J AU Laycock, S Tang, S Grindlay, J Los, E Simcoe, R Mink, D AF Laycock, S. Tang, S. Grindlay, J. Los, E. Simcoe, R. Mink, D. TI DIGITAL ACCESS TO A SKY CENTURY AT HARVARD: INITIAL PHOTOMETRY AND ASTROMETRY SO ASTRONOMICAL JOURNAL LA English DT Article DE astrometry; stars: variables: general; techniques: photometric ID GUIDE STAR CATALOG; PHOTOGRAPHIC PHOTOMETRY; PLATES AB Digital Access to a Sky Century at Harvard (DASCH) is a project to digitize the collection of similar to 500,000 glass photographic plates held at Harvard College Observatory. The collection spans the time period from 1880 to 1985, during which time every point on the sky was been observed from 500 to 1000 times. In this paper, we describe the DASCH commissioning run, during which we developed the data-reduction pipeline, characterized the plates and fine-tuned the digitizer's performance and operation. This initial run consisted of 500 plates taken from a variety of different plate series, all containing the open cluster Praeseppe (M44). We report that accurate photometry at the 0.1 mag level is possible on the majority of plates, and demonstrate century-long light curves of various types of variable stars in and around M44. DASCH will generate a public online archive of the entire plate collection, including images, source catalogs, and light curves for nearly all astronomical objects brighter than about 17th magnitude. C1 [Laycock, S.] Gemini Observ, Hilo, HI 96720 USA. [Tang, S.; Grindlay, J.; Los, E.; Simcoe, R.; Mink, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Laycock, S (reprint author), Gemini Observ, 670 N AOHoku Pl, Hilo, HI 96720 USA. EM silas@head.cfa.harvard.edu OI Mink, Jessica/0000-0003-3594-1823 FU NSF [AST-0407380] FX We thank our colleagues at Harvard and beyond who have offered advice and expertise in photographic astronomy, digitization, and software development. In particular, we thank A. Doane, G. Champine, and A. Sliski for their inestimable contributions. DASCH has been supported by NSF grant AST-0407380 for which we are grateful. S.L. acknowledges the generous support of Gemini Observatory. NR 24 TC 14 Z9 14 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 2010 VL 140 IS 4 BP 1062 EP 1077 DI 10.1088/0004-6256/140/4/1062 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 648VM UT WOS:000281722500016 ER PT J AU Bacmann, A Caux, E Hily-Blant, P Parise, B Pagani, L Bottinelli, S Maret, S Vastel, C Ceccarelli, C Cernicharo, J Henning, T Castets, A Coutens, A Bergin, EA Blake, GA Crimier, N Demyk, K Dominik, C Gerin, M Hennebelle, P Kahane, C Klotz, A Melnick, G Schilke, P Wakelam, V Walters, A Baudry, A Bell, T Benedettini, M Boogert, A Cabrit, S Caselli, P Codella, C Comito, C Encrenaz, P Falgarone, E Fuente, A Goldsmith, PF Helmich, F Herbst, E Jacq, T Kama, M Langer, W Lefloch, B Lis, D Lord, S Lorenzani, A Neufeld, D Nisini, B Pacheco, S Pearson, J Phillips, T Salez, M Saraceno, P Schuster, K Tielens, X van der Tak, FFS van der Wiel, MHD Viti, S Wyrowski, F Yorke, H Faure, A Benz, A Coeur-Joly, O Cros, A Gusten, R Ravera, L AF Bacmann, A. Caux, E. Hily-Blant, P. Parise, B. Pagani, L. Bottinelli, S. Maret, S. Vastel, C. Ceccarelli, C. Cernicharo, J. Henning, T. Castets, A. Coutens, A. Bergin, E. A. Blake, G. A. Crimier, N. Demyk, K. Dominik, C. Gerin, M. Hennebelle, P. Kahane, C. Klotz, A. Melnick, G. Schilke, P. Wakelam, V. Walters, A. Baudry, A. Bell, T. Benedettini, M. Boogert, A. Cabrit, S. Caselli, P. Codella, C. Comito, C. Encrenaz, P. Falgarone, E. Fuente, A. Goldsmith, P. F. Helmich, F. Herbst, E. Jacq, T. Kama, M. Langer, W. Lefloch, B. Lis, D. Lord, S. Lorenzani, A. Neufeld, D. Nisini, B. Pacheco, S. Pearson, J. Phillips, T. Salez, M. Saraceno, P. Schuster, K. Tielens, X. van der Tak, F. F. S. van der Wiel, M. H. D. Viti, S. Wyrowski, F. Yorke, H. Faure, A. Benz, A. Coeur-Joly, O. Cros, A. Guesten, R. Ravera, L. TI First detection of ND in the solar-mass protostar IRAS16293-2422 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: molecules; stars: formation ID DOUBLY DEUTERATED FORMALDEHYDE; STAR-FORMING REGIONS; DEUTERIUM FRACTIONATION; MOLECULAR-SPECTROSCOPY; COLOGNE DATABASE; CORES; TRANSITION; METHANOL; AMMONIA; CDMS AB Context. In the past decade, much progress has been made in characterising the processes leading to the enhanced deuterium fractionation observed in the ISM and in particular in the cold, dense parts of star forming regions such as protostellar envelopes. Very high molecular D/H ratios have been found for saturated molecules and ions. However, little is known about the deuterium fractionation in radicals, even though simple radicals often represent an intermediate stage in the formation of more complex, saturated molecules. The imidogen radical NH is such an intermediate species for the ammonia synthesis in the gas phase. Many of these light molecules however have their fundamental transitions in the submillimetre domain and their detection is hampered by the opacity of the atmosphere at these wavelengths. Herschel/HIFI represents a unique opportunity to study the deuteration and formation mechanisms of species not observable from the ground. Aims. We searched here for the deuterated radical ND in order to determine the deuterium fractionation of imidogen and constrain the deuteration mechanism of this species. Methods. We observed the solar-mass Class 0 protostar IRAS16293-2422 with the heterodyne instrument HIFI in Bands 1a (480-560 GHz), 3b (858-961 GHz), and 4a (949-1061 GHz) as part of the Herschel key programme CHESS (Chemical HErschel Survey of Star forming regions). Results. The deuterated form of the imidogen radical ND was detected and securely identified with 2 hyperfine component groups of its fundamental transition (N = 0-1) at 522.1 and 546.2 GHz, in absorption against the continuum background emitted from the nascent protostar. The 3 groups of hyperfine components of its hydrogenated counterpart NH were also detected in absorption. The absorption arises from the cold envelope, where many deuterated species have been shown to be abundant. The estimated column densities are similar to 2 x 10(14) cm(-2) for NH and similar to 1.3 x 10(14) cm(-2) for ND. We derive a very high deuterium fractionation with an [ND]/[NH] ratio of between 30 and 100%. Conclusions. The deuterium fractionation of imidogen is of the same order of magnitude as that in other molecules, which suggests that an efficient deuterium fractionation mechanism is at play. We discuss two possible formation pathways for ND, by means of either the reaction of N+ with HD, or deuteron/proton exchange with NH. C1 [Bacmann, A.; Hily-Blant, P.; Maret, S.; Ceccarelli, C.; Castets, A.; Crimier, N.; Kahane, C.; Lefloch, B.; Pacheco, S.; Faure, A.] Univ Grenoble 1, CNRS, UMR 5571, Lab Astrophys Grenoble, Grenoble, France. [Bacmann, A.; Ceccarelli, C.; Wakelam, V.; Baudry, A.] Univ Bordeaux, Lab Astrophys Bordeaux, Floirac, France. [Boogert, A.; Lord, S.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91109 USA. [Benedettini, M.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Rome, Italy. [Caux, E.; Bottinelli, S.; Vastel, C.; Coutens, A.; Demyk, K.; Klotz, A.; Walters, A.; Coeur-Joly, O.; Cros, A.; Ravera, L.] Univ Toulouse 3, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse, France. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds, W Yorkshire, England. [Pagani, L.; Cabrit, S.; Encrenaz, P.; Salez, M.] Observ Paris, LERMA, F-75014 Paris, France. [Pagani, L.; Cabrit, S.; Encrenaz, P.; Salez, M.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Cernicharo, J.; Crimier, N.] CSIC INTA, Ctr Astrobiol, Madrid, Spain. [Parise, B.; Schilke, P.; Comito, C.; Wyrowski, F.; Guesten, R.] Max Planck Inst Radioastron, D-5300 Bonn, Germany. [Codella, C.; Lorenzani, A.] INAF Osservatorio Astrofis Arcetri, Florence, Italy. [Dominik, C.; Kama, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6525 ED Nijmegen, Netherlands. [Fuente, A.] IGN Observ Astron Nacl, Alcala De Henares, Spain. [Goldsmith, P. F.; Langer, W.; Pearson, J.; Yorke, H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Helmich, F.; van der Tak, F. F. S.; van der Wiel, M. H. D.] SRON Netherlands Inst Space Res, Groningen, Netherlands. [Herbst, E.] Ohio State Univ, Columbus, OH 43210 USA. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neufeld, D.] Johns Hopkins Univ, Baltimore, MD USA. [Schilke, P.] Univ Cologne, Inst Phys, Cologne, Germany. [Schuster, K.] Inst Radio Astron Millimetr, Grenoble, France. [Tielens, X.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Viti, S.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Nisini, B.] INAF Osservatorio Astron Roma, Monte Porzio Catone, Italy. [Bergin, E. A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [van der Tak, F. F. S.; van der Wiel, M. H. D.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands. [Gerin, M.; Hennebelle, P.; Falgarone, E.; Salez, M.] UCP, UPMC, ENS,UMR CNRS INSU 8112, OP,Lab Etud Rayonnement & Matiere Astrophys, Paris, France. [Caux, E.; Bottinelli, S.; Vastel, C.; Coutens, A.; Demyk, K.; Klotz, A.; Walters, A.; Coeur-Joly, O.; Cros, A.; Ravera, L.] CNRS INSU, UMR 5187, Toulouse, France. [Bacmann, A.; Ceccarelli, C.; Wakelam, V.; Baudry, A.; Jacq, T.] CNRS INSU, UMR 5804, Floirac, France. [Benz, A.] ETH, Inst Astron, CH-8092 Zurich, Switzerland. RP Bacmann, A (reprint author), Univ Grenoble 1, CNRS, UMR 5571, Lab Astrophys Grenoble, Grenoble, France. EM aurore.bacmann@obs.ujf-grenoble.fr RI van der Wiel, Matthijs/M-4531-2014; Coutens, Audrey/M-4533-2014; Fuente, Asuncion/G-1468-2016; Goldsmith, Paul/H-3159-2016; OI van der Wiel, Matthijs/0000-0002-4325-3011; Coutens, Audrey/0000-0003-1805-3920; Fuente, Asuncion/0000-0001-6317-6343; Lorenzani, Andrea/0000-0002-4685-3434; Wakelam, Valentine/0000-0001-9676-2605; Kama, Mihkel/0000-0003-0065-7267; Codella, Claudio/0000-0003-1514-3074; , Brunella Nisini/0000-0002-9190-0113; Maret, Sebastien/0000-0003-1104-4554 NR 32 TC 26 Z9 26 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L42 DI 10.1051/0004-6361/201015102 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900042 ER PT J AU Benz, AO Bruderer, S van Dishoeck, EF Stauber, P Wampfler, SF Melchior, M Dedes, C Wyrowski, F Doty, SD van der Tak, F Bachtold, W Csillaghy, A Megej, A Monstein, C Soldati, M Bachiller, R Baudry, A Benedettini, M Bergin, E Bjerkeli, P Blake, GA Bontemps, S Braine, J Caselli, P Cernicharo, J Codella, C Daniel, F di Giorgio, AM Dieleman, P Dominik, C Encrenaz, P Fich, M Fuente, A Giannini, T Goicoechea, JR de Graauw, T Helmich, F Herczeg, GJ Herpin, F Hogerheijde, MR Jacq, T Jellema, W Johnstone, D Jorgensen, JK Kristensen, LE Larsson, B Lis, D Liseau, R Marseille, M McCoey, C Melnick, G Neufeld, D Nisini, B Olberg, M Ossenkopf, V Parise, B Pearson, JC Plume, R Risacher, C Santiago-Garcia, J Saraceno, P Schieder, R Shipman, R Stutzki, J Tafalla, M Tielens, AGGM van Kempen, TA Visser, R Yildiz, UA AF Benz, A. O. Bruderer, S. van Dishoeck, E. F. Staeuber, P. Wampfler, S. F. Melchior, M. Dedes, C. Wyrowski, F. Doty, S. D. van der Tak, F. Baechtold, W. Csillaghy, A. Megej, A. Monstein, C. Soldati, M. Bachiller, R. Baudry, A. Benedettini, M. Bergin, E. Bjerkeli, P. Blake, G. A. Bontemps, S. Braine, J. Caselli, P. Cernicharo, J. Codella, C. Daniel, F. di Giorgio, A. M. Dieleman, P. Dominik, C. Encrenaz, P. Fich, M. Fuente, A. Giannini, T. Goicoechea, J. R. de Graauw, Th. Helmich, F. Herczeg, G. J. Herpin, F. Hogerheijde, M. R. Jacq, T. Jellema, W. Johnstone, D. Jorgensen, J. K. Kristensen, L. E. Larsson, B. Lis, D. Liseau, R. Marseille, M. McCoey, C. Melnick, G. Neufeld, D. Nisini, B. Olberg, M. Ossenkopf, V. Parise, B. Pearson, J. C. Plume, R. Risacher, C. Santiago-Garcia, J. Saraceno, P. Schieder, R. Shipman, R. Stutzki, J. Tafalla, M. Tielens, A. G. G. M. van Kempen, T. A. Visser, R. Yildiz, U. A. TI Hydrides in young stellar objects: Radiation tracers in a protostar-disk-outflow system SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; line: identification; stars: formation; stars: massive; photon-dominated region; submillimeter: ISM ID H2O+; SPECTROSCOPY; CHEMISTRY; REGIONS; W3IRS5; DR21; H3O+ AB Context. Hydrides of the most abundant heavier elements are fundamental molecules in cosmic chemistry. Some of them trace gas irradiated by UV or X-rays. Aims. We explore the abundances of major hydrides in W3 IRS5, a prototypical region of high-mass star formation. Methods. W3 IRS5 was observed by HIFI on the Herschel Space Observatory with deep integration (similar or equal to 2500 s) in 8 spectral regions. Results. The target lines including CH, NH, H3O+, and the new molecules SH+, H2O+, and OH+ are detected. The H2O+ and OH+ J = 1-0 lines are found mostly in absorption, but also appear to exhibit weak emission (P-Cyg-like). Emission requires high density, thus originates most likely near the protostar. This is corroborated by the absence of line shifts relative to the young stellar object (YSO). In addition, H2O+ and OH+ also contain strong absorption components at a velocity shifted relative to W3 IRS5, which are attributed to foreground clouds. Conclusions. The molecular column densities derived from observations correlate well with the predictions of a model that assumes the main emission region is in outflow walls, heated and irradiated by protostellar UV radiation. C1 [Benz, A. O.; Bruderer, S.; Staeuber, P.; Wampfler, S. F.; Melchior, M.; Dedes, C.; Monstein, C.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [van Dishoeck, E. F.; Hogerheijde, M. R.; Kristensen, L. E.; Tielens, A. G. G. M.; Visser, R.; Yildiz, U. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.; Herczeg, G. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Caselli, P.; Codella, C.; Jacq, T.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.] CNRS INSU, UMR 5804, Floirac, France. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Bjerkeli, P.; Liseau, R.; Olberg, M.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [van der Tak, F.; Dieleman, P.; de Graauw, Th.; Helmich, F.; Jellema, W.; Marseille, M.; Risacher, C.; Shipman, R.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [van der Tak, F.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Bachiller, R.; Tafalla, M.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Benedettini, M.; di Giorgio, A. M.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Bergin, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [Encrenaz, P.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Fuente, A.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Giannini, T.; Nisini, B.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Lis, D.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [McCoey, C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Melnick, G.; van Kempen, T. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neufeld, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Wyrowski, F.; Parise, B.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Santiago-Garcia, J.] Inst Radio Astron Millimetr, Granada 18012, Spain. [Ossenkopf, V.; Schieder, R.; Stutzki, J.] Univ Cologne, Inst Phys 1, KOSMA, D-50937 Cologne, Germany. [Melchior, M.; Csillaghy, A.; Soldati, M.] Univ Appl Sci NW, Inst Technol 4D, CH-5210 Windisch, Switzerland. [Baechtold, W.; Megej, A.] ETH, Lab Electromagnet Fields & Microwave Elect, CH-8092 Zurich, Switzerland. RP Benz, AO (reprint author), ETH, Inst Astron, CH-8093 Zurich, Switzerland. EM benz@astro.phys.ethz.ch RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Jorgensen, Jes Kristian/L-7936-2014; Wampfler, Susanne/D-2270-2015; Fuente, Asuncion/G-1468-2016; OI Giannini, Teresa/0000-0002-0224-096X; Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Jorgensen, Jes Kristian/0000-0001-9133-8047; Wampfler, Susanne/0000-0002-3151-7657; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118; Codella, Claudio/0000-0003-1514-3074; , Brunella Nisini/0000-0002-9190-0113 FU Swiss National Science Foundation [200020-113556] FX We thank Michael Kaufman and Serena Viti for helpful comments on an early draft. This program is made possible thanks to the Swiss Herschel guaranteed time program. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research Groningen, The Netherlands and with major contributions from Germany, France, and the US. Consortium members are: Canada:CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland: NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INT); Sweden: Chalmers University of Technology, Onsala Space Observatory, Swedish National Space Board, Stockholm University; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. The work on star formation at ETH Zurich is partially funded by the Swiss National Science Foundation (grant no. 200020-113556). NR 27 TC 44 Z9 44 U1 1 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L35 DI 10.1051/0004-6361/201015111 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900035 ER PT J AU Bergin, EA Phillips, TG Comito, C Crockett, NR Lis, DC Schilke, P Wang, S Bell, TA Blake, GA Bumble, B Caux, E Cabrit, S Ceccarelli, C Cernicharo, J Daniel, F de Graauw, T Dubernet, ML Emprechtinger, M Encrenaz, P Falgarone, E Gerin, M Giesen, TF Goicoechea, JR Goldsmith, PF Gupta, H Hartogh, P Helmich, FP Herbst, E Joblin, C Johnstone, D Kawamura, JH Langer, WD Latter, WB Lord, SD Maret, S Martin, PG Melnick, GJ Menten, KM Morris, P Muller, HSP Murphy, JA Neufeld, DA Ossenkopf, V Pagani, L Pearson, JC Perault, M Plume, R Roelfsema, P Qin, SL Salez, M Schlemmer, S Stutzki, J Tielens, AGGM Trappe, N van der Tak, FFS Vastel, C Yorke, HW Yu, S Zmuidzinas, J AF Bergin, E. A. Phillips, T. G. Comito, C. Crockett, N. R. Lis, D. C. Schilke, P. Wang, S. Bell, T. A. Blake, G. A. Bumble, B. Caux, E. Cabrit, S. Ceccarelli, C. Cernicharo, J. Daniel, F. de Graauw, Th. Dubernet, M. -L. Emprechtinger, M. Encrenaz, P. Falgarone, E. Gerin, M. Giesen, T. F. Goicoechea, J. R. Goldsmith, P. F. Gupta, H. Hartogh, P. Helmich, F. P. Herbst, E. Joblin, C. Johnstone, D. Kawamura, J. H. Langer, W. D. Latter, W. B. Lord, S. D. Maret, S. Martin, P. G. Melnick, G. J. Menten, K. M. Morris, P. Mueller, H. S. P. Murphy, J. A. Neufeld, D. A. Ossenkopf, V. Pagani, L. Pearson, J. C. Perault, M. Plume, R. Roelfsema, P. Qin, S. -L. Salez, M. Schlemmer, S. Stutzki, J. Tielens, A. G. G. M. Trappe, N. van der Tak, F. F. S. Vastel, C. Yorke, H. W. Yu, S. Zmuidzinas, J. TI Herschel observations of EXtra-Ordinary Sources (HEXOS): The present and future of spectral surveys with Herschel/ HIFI SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: abundances; ISM: molecules; submillimeter: ISM ID LINE SURVEY; ORION KL; MOLECULAR-SPECTROSCOPY; COLOGNE DATABASE; HOT CORES; WATER; SUBMILLIMETER; GHZ; CLOUDS; BAND AB We present initial results from the Herschel GT key program: Herschel observations of EXtra-Ordinary Sources (HEXOS) and outline the promise and potential of spectral surveys with Herschel/HIFI. The HIFI instrument offers unprecedented sensitivity, as well as continuous spectral coverage across the gaps imposed by the atmosphere, opening up a largely unexplored wavelength regime to high-resolution spectroscopy. We show the spectrum of Orion KL between 480 and 560 GHz and from 1.06 to 1.115 THz. From these data, we confirm that HIFI separately measures the dust continuum and spectrally resolves emission lines in Orion KL. Based on this capability we demonstrate that the line contribution to the broad-band continuum in this molecule-rich source is similar to 20-40% below 1 THz and declines to a few percent at higher frequencies. We also tentatively identify multiple transitions of (HDO)-O-18 in the spectra. The first detection of this rare isotopologue in the interstellar medium suggests that HDO emission is optically thick in the Orion hot core with HDO/H2O similar to 0.02. We discuss the implications of this detection for the water D/H ratio in hot cores. C1 [Bergin, E. A.; Crockett, N. R.; Wang, S.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Phillips, T. G.; Lis, D. C.; Bell, T. A.; Emprechtinger, M.; Zmuidzinas, J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Comito, C.; Schilke, P.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Schilke, P.; Giesen, T. F.; Mueller, H. S. P.; Ossenkopf, V.; Qin, S. -L.; Schlemmer, S.; Stutzki, J.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Bumble, B.; Goldsmith, P. F.; Gupta, H.; Kawamura, J. H.; Langer, W. D.; Pearson, J. C.; Yorke, H. W.; Yu, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Caux, E.; Joblin, C.; Vastel, C.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.; Joblin, C.; Vastel, C.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Cabrit, S.; Pagani, L.; Salez, M.] LERMA, F-75014 Paris, France. [Ceccarelli, C.; Maret, S.] Lab Astrophys Observ Grenoble, F-38041 Grenoble 9, France. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Madrid 28850, Spain. [Cabrit, S.; Pagani, L.; Salez, M.] Observ Paris, CNRS, UMR8112, F-75014 Paris, France. [Daniel, F.; Encrenaz, P.; Falgarone, E.; Gerin, M.; Perault, M.] Observ Paris, UMR8112, CNRS, LERMA, F-75231 Paris 05, France. [Daniel, F.; Encrenaz, P.; Falgarone, E.; Gerin, M.; Perault, M.] Ecole Normale Super, F-75231 Paris 05, France. [de Graauw, Th.; Helmich, F. P.; Ossenkopf, V.; Roelfsema, P.; van der Tak, F. F. S.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Dubernet, M. -L.] Univ Paris 06, LPMAA, UMR7092, Paris, France. [Dubernet, M. -L.] Observ Paris, LUTH, UMR8102, Meudon, France. [Hartogh, P.] MPI Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Latter, W. B.; Lord, S. D.; Morris, P.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murphy, J. A.; Trappe, N.] Natl Univ Ireland Maynooth, Maynooth, Kildare, Ireland. [Neufeld, D. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Tielens, A. G. G. M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Bergin, EA (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM ebergin@umich.edu RI Giesen, Thomas /B-9476-2015; Schlemmer, Stephan/E-2903-2015; Trappe, Neil/C-9014-2016; Yu, Shanshan/D-8733-2016; Goldsmith, Paul/H-3159-2016; OI Maret, Sebastien/0000-0003-1104-4554; Giesen, Thomas /0000-0002-2401-0049; Schlemmer, Stephan/0000-0002-1421-7281; Trappe, Neil/0000-0003-2527-9821; Mueller, Holger/0000-0002-0183-8927 FU NASA FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada, and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands, and with major contributions from Germany, France, and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri -INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio AstronU mico Nacional (IGN), Centro de AstrobiologSa (CSIC-INTA). Sweden: Chalmers University of Technology -MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University -Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. The HEXOS team also is grateful to the HIFI instrument team for building a fantastic instrument. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 29 TC 73 Z9 73 U1 0 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L20 DI 10.1051/0004-6361/201015071 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900020 ER PT J AU Bergin, EA Hogerheijde, MR Brinch, C Fogel, J Yildiz, UA Kristensen, LE van Dishoeck, EF Bell, TA Blake, GA Cernicharo, J Dominik, C Lis, D Melnick, G Neufeld, D Panic, O Pearson, JC Bachiller, R Baudry, A Benedettini, M Benz, AO Bjerkeli, P Bontemps, S Braine, J Bruderer, S Caselli, P Codella, C Daniel, F di Giorgio, AM Doty, SD Encrenaz, P Fich, M Fuente, A Giannini, T Goicoechea, JR de Graauw, T Helmich, F Herczeg, GJ Herpin, F Jacq, T Johnstone, D Jorgensen, JK Larsson, B Liseau, R Marseille, M Mc Coey, C Nisini, B Olberg, M Parise, B Plume, R Risacher, C Santiago-Garcia, J Saraceno, P Shipman, R Tafalla, M van Kempen, TA Visser, R Wampfler, SF Wyrowski, F van der Tak, F Jellema, W Tielens, AGGM Hartogh, P Stutzki, J Szczerba, R AF Bergin, E. A. Hogerheijde, M. R. Brinch, C. Fogel, J. Yildiz, U. A. Kristensen, L. E. van Dishoeck, E. F. Bell, T. A. Blake, G. A. Cernicharo, J. Dominik, C. Lis, D. Melnick, G. Neufeld, D. Panic, O. Pearson, J. C. Bachiller, R. Baudry, A. Benedettini, M. Benz, A. O. Bjerkeli, P. Bontemps, S. Braine, J. Bruderer, S. Caselli, P. Codella, C. Daniel, F. di Giorgio, A. M. Doty, S. D. Encrenaz, P. Fich, M. Fuente, A. Giannini, T. Goicoechea, J. R. de Graauw, Th Helmich, F. Herczeg, G. J. Herpin, F. Jacq, T. Johnstone, D. Jorgensen, J. K. Larsson, B. Liseau, R. Marseille, M. Mc Coey, C. Nisini, B. Olberg, M. Parise, B. Plume, R. Risacher, C. Santiago-Garcia, J. Saraceno, P. Shipman, R. Tafalla, M. van Kempen, T. A. Visser, R. Wampfler, S. F. Wyrowski, F. van der Tak, F. Jellema, W. Tielens, A. G. G. M. Hartogh, P. Stuetzki, J. Szczerba, R. TI Sensitive limits on the abundance of cold water vapor in the DM Tauri protoplanetary disk SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: abundances; ISM: molecules; protoplanetary disks ID PLANET-FORMING REGION; CIRCUMSTELLAR DISKS; H2O; STARS; DUST; MOLECULES; SPECTRA; GAS; DESORPTION; EVOLUTION AB We performed a sensitive search for the ground-state emission lines of ortho-and para-water vapor in the DM Tau protoplanetary disk using the Herschel/HIFI instrument. No strong lines are detected down to 3 sigma levels in 0.5 km s(-1) channels of 4.2 mK for the 1(10)-1(01) line and 12.6 mK for the 1(11)-0(00) line. We report a very tentative detection, however, of the 1(10)-1(01) line in the wide band spectrometer, with a strength of T-mb = 2.7 mK, a width of 5.6 km s(-1) and an integrated intensity of 16.0 mK km s(-1). The latter constitutes a 6 sigma detection. Regardless of the reality of this tentative detection, model calculations indicate that our sensitive limits on the line strengths preclude efficient desorption of water in the UV illuminated regions of the disk. We hypothesize that more than 95-99% of the water ice is locked up in coagulated grains that have settled to the midplane. C1 [Bergin, E. A.; Fogel, J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Hogerheijde, M. R.; Brinch, C.; Yildiz, U. A.; Kristensen, L. E.; van Dishoeck, E. F.; Visser, R.; Tielens, A. G. G. M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.; Herczeg, G. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] CSIC INTA, Ctr Astrobiol, Dept Astrofis, Madrid 28850, Spain. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Bell, T. A.; Lis, D.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Melnick, G.; van Kempen, T. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neufeld, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Panic, O.] European So Observ, D-85748 Garching, Germany. [Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bachiller, R.; Tafalla, M.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Baudry, A.; di Giorgio, A. M.; Herpin, F.; Nisini, B.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Benedettini, M.; Caselli, P.; Codella, C.; Jacq, T.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Benz, A. O.; Bruderer, S.; Wampfler, S. F.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Bjerkeli, P.; Liseau, R.; Olberg, M.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [Bontemps, S.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Bontemps, S.] CNRS INSU, UMR 5804, Floirac, France. [Braine, J.; Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [Fich, M.; Mc Coey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Fuente, A.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Giannini, T.] INAF Osservatorio Astronom Roma, I-00040 Monte Porzio Catone, Italy. [de Graauw, Th; Helmich, F.; Marseille, M.; Risacher, C.; Shipman, R.; van der Tak, F.; Jellema, W.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Mc Coey, C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Parise, B.; Wyrowski, F.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Santiago-Garcia, J.] Inst Radio Astron Millimetr, Granada 18012, Spain. [van der Tak, F.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Hartogh, P.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Stuetzki, J.] Univ Cologne, Inst Phys 1, KOSMA, D-50937 Cologne, Germany. [Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. RP Bergin, EA (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM ebergin@umich.edu RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Wampfler, Susanne/D-2270-2015; Brinch, Christian/G-5157-2015; Fuente, Asuncion/G-1468-2016; OI Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Wampfler, Susanne/0000-0002-3151-7657; Brinch, Christian/0000-0002-5074-7183; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118; Codella, Claudio/0000-0003-1514-3074; Giannini, Teresa/0000-0002-0224-096X; , Brunella Nisini/0000-0002-9190-0113 FU NASA through JPL/Caltech; NSF [0707777]; NWO [639.042.404] FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. E.A.B. acknowledges support by NSF Grant 0707777, M.R.H. by NWO grant 639.042.404. NR 37 TC 42 Z9 42 U1 1 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L33 DI 10.1051/0004-6361/201015104 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900033 ER PT J AU Bruderer, S Benz, AO van Dishoeck, EF Melchior, M Doty, SD van der Tak, F Stauber, P Wampfler, SF Dedes, C Yildiz, UA Pagani, L Giannini, T de Graauw, T Whyborn, N Teyssier, D Jellema, W Shipman, R Schieder, R Honingh, N Caux, E Bachtold, W Csillaghy, A Monstein, C Bachiller, R Baudry, A Benedettini, M Bergin, E Bjerkeli, P Blake, GA Bontemps, S Braine, J Caselli, P Cernicharo, J Codella, C Daniel, F di Giorgio, AM Dominik, C Encrenaz, P Fich, M Fuente, A Goicoechea, JR Helmich, F Herczeg, GJ Herpin, F Hogerheijde, MR Jacq, T Johnstone, D Jorgensen, JK Kristensen, LE Larsson, B Lis, D Liseau, R Marseille, M McCoey, C Melnick, G Neufeld, D Nisini, B Olberg, M Parise, B Pearson, JC Plume, R Risacher, C Santiago-Garcia, J Saraceno, P Shipman, R Tafalla, M van Kempen, TA Visser, R Wyrowski, F AF Bruderer, S. Benz, A. O. van Dishoeck, E. F. Melchior, M. Doty, S. D. van der Tak, F. Staeuber, P. Wampfler, S. F. Dedes, C. Yildiz, U. A. Pagani, L. Giannini, T. de Graauw, Th. Whyborn, N. Teyssier, D. Jellema, W. Shipman, R. Schieder, R. Honingh, N. Caux, E. Baechtold, W. Csillaghy, A. Monstein, C. Bachiller, R. Baudry, A. Benedettini, M. Bergin, E. Bjerkeli, P. Blake, G. A. Bontemps, S. Braine, J. Caselli, P. Cernicharo, J. Codella, C. Daniel, F. di Giorgio, A. M. Dominik, C. Encrenaz, P. Fich, M. Fuente, A. Goicoechea, J. R. Helmich, F. Herczeg, G. J. Herpin, F. Hogerheijde, M. R. Jacq, T. Johnstone, D. Jorgensen, J. K. Kristensen, L. E. Larsson, B. Lis, D. Liseau, R. Marseille, M. McCoey, C. Melnick, G. Neufeld, D. Nisini, B. Olberg, M. Parise, B. Pearson, J. C. Plume, R. Risacher, C. Santiago-Garcia, J. Saraceno, P. Shipman, R. Tafalla, M. van Kempen, T. A. Visser, R. Wyrowski, F. TI Herschel/HIFI detections of hydrides towards AFGL 2591 Envelope emission versus tenuous cloud absorption SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: molecules; stars: formation; astrochemistry; ISM: individual objects: AFGL 2591 ID STAR-FORMING REGIONS; INTERSTELLAR-MEDIUM; OUTFLOW; CHEMISTRY; SPECTROSCOPY; GL-2591; H2O+; EXCITATION; ABUNDANCE AB The Heterodyne Instrument for the Far Infrared (HIFI) onboard the Herschel Space Observatory allows the first observations of light diatomic molecules at high spectral resolution and in multiple transitions. Here, we report deep integrations using HIFI in different lines of hydrides towards the high-mass star forming region AFGL 2591. Detected are CH, CH+, NH, OH+, H2O+, while NH+ and SH+ have not been detected. All molecules except for CH and CH+ are seen in absorption with low excitation temperatures and at velocities different from the systemic velocity of the protostellar envelope. Surprisingly, the CH(J(F,P) = 3/2(2),(-) - 1/2(1,+)) and CH+(J = 1-0, J = 2-1) lines are detected in emission at the systemic velocity. We can assign the absorption features to a foreground cloud and an outflow lobe, while the CH and CH+ emission stems from the envelope. The observed abundance and excitation of CH and CH+ can be explained in the scenario of FUV irradiated outflow walls, where a cavity etched out by the outflow allows protostellar FUV photons to irradiate and heat the envelope at larger distances driving the chemical reactions that produce these molecules. C1 [Bruderer, S.; Benz, A. O.; Staeuber, P.; Wampfler, S. F.; Dedes, C.; Monstein, C.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [van Dishoeck, E. F.; Yildiz, U. A.; Hogerheijde, M. R.; Kristensen, L. E.; Visser, R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.; Herczeg, G. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Melchior, M.; Csillaghy, A.] FHNW, Inst Technol 4D, CH-5210 Windisch, Switzerland. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [van der Tak, F.; Jellema, W.; Shipman, R.; Helmich, F.; Marseille, M.; Risacher, C.; Shipman, R.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [van der Tak, F.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Pagani, L.] Observ Paris, LERMA, F-75014 Paris, France. [Giannini, T.; Nisini, B.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Pagani, L.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [de Graauw, Th.; Whyborn, N.] Joint ALMA Off, Santiago, Chile. [Teyssier, D.] ESA, European Space Astron Ctr, Madrid 28691, Spain. [Schieder, R.; Honingh, N.] Univ Cologne, Inst Phys 1, KOSMA, D-50937 Cologne, Germany. [Caux, E.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Baechtold, W.] ETH, Lab Electromagnet Fields Ad Microwave Elect, CH-8092 Zurich, Switzerland. [Bachiller, R.; Tafalla, M.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.] CNRS INSU, UMR 5804, Floirac, France. [Benedettini, M.; di Giorgio, A. M.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Bergin, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bjerkeli, P.; Liseau, R.; Olberg, M.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Caselli, P.; Codella, C.; Jacq, T.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] CSIC INTA, Ctr Astrobiol, Dept Astrofis, Madrid 28850, Spain. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Fuente, A.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Lis, D.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [McCoey, C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Melnick, G.; van Kempen, T. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neufeld, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Parise, B.; Wyrowski, F.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Santiago-Garcia, J.] IRAM, E-18012 Granada, Spain. RP Bruderer, S (reprint author), ETH, Inst Astron, CH-8093 Zurich, Switzerland. EM simonbr@astro.phys.ethz.ch RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Jorgensen, Jes Kristian/L-7936-2014; Wampfler, Susanne/D-2270-2015; Fuente, Asuncion/G-1468-2016; OI Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Jorgensen, Jes Kristian/0000-0001-9133-8047; Wampfler, Susanne/0000-0002-3151-7657; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118; Codella, Claudio/0000-0003-1514-3074; Giannini, Teresa/0000-0002-0224-096X; , Brunella Nisini/0000-0002-9190-0113 FU Swiss National Science Foundation [200020-113556] FX We thank the anonymous referee for useful comments. The work on star formation at ETH Zurich is partially funded by the Swiss National Science Foundation grant 200020-113556. This program is made possible thanks to the Swiss HIFI guaranteed time program. HIFI has been designed and built by a consortium of institutes and university departments from acrossEurope, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologa (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. HIPE is a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS and SPIRE consortia. NR 27 TC 31 Z9 31 U1 1 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L44 DI 10.1051/0004-6361/201015098 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900044 ER PT J AU Bujarrabal, V Alcolea, J Soria-Ruiz, R Planesas, P Teyssier, D Marston, AP Cernicharo, J Decin, L Dominik, C Justtanont, K de Koter, A Melnick, G Menten, KM Neufeld, DA Olofsson, H Schmidt, M Schoier, FL Szczerba, R Waters, LBFM Quintana-Lacaci, G Gusten, R Gallego, JD Diez-Gonzalez, MC Barcia, A Lopez-Fernandez, I Wildeman, K Tielens, AGGM Jacobs, K AF Bujarrabal, V. Alcolea, J. Soria-Ruiz, R. Planesas, P. Teyssier, D. Marston, A. P. Cernicharo, J. Decin, L. Dominik, C. Justtanont, K. de Koter, A. Melnick, G. Menten, K. M. Neufeld, D. A. Olofsson, H. Schmidt, M. Schoier, F. L. Szczerba, R. Waters, L. B. F. M. Quintana-Lacaci, G. Guesten, R. Gallego, J. D. Diez-Gonzalez, M. C. Barcia, A. Lopez-Fernandez, I. Wildeman, K. Tielens, A. G. G. M. Jacobs, K. TI Herschel/HIFI observations of high-J CO transitions in the protoplanetary nebula CRL 618 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: AGB and post-AGB; circumstellar matter; stars: mass-loss; planetary nebulae: general; planetary nebulae: individual: CRL 618 ID HETERODYNE INSTRUMENT; MOLECULAR ENVELOPE; CRL-618; DYNAMICS; FACILITY; APEX AB Aims. We aim to study the physical conditions, particularly the excitation state, of the intermediate-temperature gas components in the protoplanetary nebula CRL 618. These components are particularly important for understanding the evolution of the nebula. Methods. We performed Herschel/HIFI observations of several CO lines in the far-infrared/sub-mm in the protoplanetary nebula CRL 618. The high spectral resolution provided by HIFI allows measurement of the line profiles. Since the dynamics and structure of the nebula is well known from mm-wave interferometric maps, it is possible to identify the contributions of the different nebular components (fast bipolar outflows, double shells, compact slow shell) to the line profiles. The observation of these relatively high-energy transitions allows an accurate study of the excitation conditions in these components, particularly in the warm ones, which cannot be properly studied from the low-energy lines. Results. The (CO)-C-12 J = 16-15, 10-9, and 6-5 lines are easily detected in this source. Both (CO)-C-13 J = 10-9 and 6-5 are also detected. Wide profiles showing spectacular line wings have been found, particularly in (CO)-C-12 J = 16-15. Other lines observed simultaneously with CO are also shown. Our analysis of the CO high-J transitions, when compared with the existing models, confirms the very low expansion velocity of the central, dense component, which probably indicates that the shells ejected during the last AGB phases were driven by radiation pressure under a regime of maximum transfer of momentum. No contribution of the diffuse halo found from mm-wave data is identified in our spectra, because of its low temperature. We find that the fast bipolar outflow is quite hot, much hotter than previously estimated; for instance, gas flowing at 100 km s(-1) must have a temperature higher than similar to 200 K. Probably, this very fast outflow, with a kinematic age < 100 yr, has been accelerated by a shock and has not yet cooled down. The double empty shell found from mm-wave mapping must also be relatively hot, in agreement with the previous estimate. C1 [Bujarrabal, V.; Planesas, P.] Observ Astron Nacl IGN, Alcala De Henares 28803, Spain. [Alcolea, J.; Soria-Ruiz, R.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Cernicharo, J.] CSIC, INTA, CAB, Madrid 28850, Spain. [Decin, L.; Waters, L. B. F. M.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium. [Decin, L.; Dominik, C.; de Koter, A.; Waters, L. B. F. M.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Justtanont, K.; Olofsson, H.; Schoier, F. L.] Chalmers, Dept Radio & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Teyssier, D.; Marston, A. P.] ESA, European Space Astron Ctr, Madrid, Spain. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Menten, K. M.; Guesten, R.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Neufeld, D. A.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Olofsson, H.] Stockholm Univ, Dept Astron, AlbaNova Univ Ctr, S-10691 Stockholm, Sweden. [Planesas, P.] Joint ALMA Observ, Santiago, Chile. [Schmidt, M.; Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6525 ED Nijmegen, Netherlands. [de Koter, A.] Univ Utrecht, Astron Inst, NL-3584 CC Utrecht, Netherlands. [Quintana-Lacaci, G.] IRAM, E-18012 Granada, Spain. [Gallego, J. D.; Diez-Gonzalez, M. C.; Barcia, A.; Lopez-Fernandez, I.] Ctr Astron Yebes, Observ Astron Nacl IGN, E-19080 Guadalajara, Spain. [Wildeman, K.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Tielens, A. G. G. M.] Leiden Univ, NL-2300 RA Leiden, Netherlands. [Jacobs, K.] Univ Cologne, KOSMA, Inst Phys 1, D-50937 Cologne, Germany. RP Bujarrabal, V (reprint author), Observ Astron Nacl IGN, Ap 112, Alcala De Henares 28803, Spain. EM v.bujarrabal@oan.es RI Planesas, Pere/G-7950-2015; OI Planesas, Pere/0000-0002-7808-3040; /0000-0003-1689-9201; Quintana-Lacaci, Guillermo/0000-0002-5417-1943 FU Spanish MICINN [CSD2009-00038]; Polish MNiSW [N 203 393334]; SNSB; MICINN [AYA2009-07304]; National Aeronautics and Space Administration FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada, and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands, and with major contributions from Germany, France, and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri- INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, J.P.L., NHSC. HCSS / HSpot / HIPE is a joint development (are joint developments) by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS, and SPIRE consortia. This work has been partially supported by the Spanish MICINN, program CONSOLIDER INGENIO 2010, grant "ASTROMOL" (CSD2009-00038). R.Sz. and M.Sch. acknowledge support from grant N 203 393334 from the Polish MNiSW. K.J. acknowledges the funding from SNSB. J.C. acknowledges funding from MICINN, grant AYA2009-07304. This research was performed, in part, through a JPL contract funded by the National Aeronautics and Space Administration. NR 16 TC 21 Z9 21 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L3 DI 10.1051/0004-6361/201015068 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900003 ER PT J AU Caselli, P Keto, E Pagani, L Aikawa, Y Yildiz, UA van der Tak, FFS Tafalla, M Bergin, EA Nisini, B Codella, C van Dishoeck, EF Bachiller, R Baudry, A Benedettini, M Benz, AO Bjerkeli, P Blake, GA Bontemps, S Braine, J Bruderer, S Cernicharo, J Daniel, F di Giorgio, AM Dominik, C Doty, SD Encrenaz, P Fich, M Fuente, A Gaier, T Giannini, T Goicoechea, JR de Graauw, T Helmich, F Herczeg, GJ Herpin, F Hogerheijde, MR Jackson, B Jacq, T Javadi, H Johnstone, D Jorgensen, JK Kester, D Kristensen, LE Laauwen, W Larsson, B Lis, D Liseau, R Luinge, W Marseille, M McCoey, C Megej, A Melnick, G Neufeld, D Olberg, M Parise, B Pearson, JC Plume, R Risacher, C Santiago-Garcia, J Saraceno, P Shipman, R Siegel, P van Kempen, TA Visser, R Wampfler, SF Wyrowski, F AF Caselli, P. Keto, E. Pagani, L. Aikawa, Y. Yildiz, U. A. van der Tak, F. F. S. Tafalla, M. Bergin, E. A. Nisini, B. Codella, C. van Dishoeck, E. F. Bachiller, R. Baudry, A. Benedettini, M. Benz, A. O. Bjerkeli, P. Blake, G. A. Bontemps, S. Braine, J. Bruderer, S. Cernicharo, J. Daniel, F. di Giorgio, A. M. Dominik, C. Doty, S. D. Encrenaz, P. Fich, M. Fuente, A. Gaier, T. Giannini, T. Goicoechea, J. R. de Graauw, Th. Helmich, F. Herczeg, G. J. Herpin, F. Hogerheijde, M. R. Jackson, B. Jacq, T. Javadi, H. Johnstone, D. Jorgensen, J. K. Kester, D. Kristensen, L. E. Laauwen, W. Larsson, B. Lis, D. Liseau, R. Luinge, W. Marseille, M. McCoey, C. Megej, A. Melnick, G. Neufeld, D. Olberg, M. Parise, B. Pearson, J. C. Plume, R. Risacher, C. Santiago-Garcia, J. Saraceno, P. Shipman, R. Siegel, P. van Kempen, T. A. Visser, R. Wampfler, S. F. Wyrowski, F. TI Water vapor toward starless cores: The Herschel view SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; line: formation; molecular processes; radiative transfer; stars: formation; ISM: clouds ID DENSE INTERSTELLAR CLOUDS; PRE-STELLAR CORES; MOLECULAR-IONS; INITIAL CONDITIONS; PRESTELLAR CORES; ABUNDANCE; L1544; TEMPERATURE; DEPLETION; OXYGEN AB Aims. Previous studies by the satellites SWAS and Odin provided stringent upper limits on the gas phase water abundance of dark clouds (x(H2O) < 7 x 10(-9)). We investigate the chemistry of water vapor in starless cores beyond the previous upper limits using the highly improved angular resolution and sensitivity of Herschel and measure the abundance of water vapor during evolutionary stages just preceding star formation. Methods. High spectral resolution observations of the fundamental ortho water (o-H2O) transition (557 GHz) were carried out with the Heterodyne Instrument for the Far Infrared onboard Herschel toward two starless cores: Barnard 68 (hereafter B68), a Bok globule, and LDN 1544 (L1544), a prestellar core embedded in the Taurus molecular cloud complex. Detailed radiative transfer and chemical codes were used to analyze the data. Results. The RMS in the brightness temperature measured for the B68 and L1544 spectra is 2.0 and 2.2 mK, respectively, in a velocity bin of 0.59 km s(-1). The continuum level is 3.5 +/- 0.2 mK in B68 and 11.4 +/- 0.4 mK in L1544. No significant feature is detected in B68 and the 3 sigma upper limit is consistent with a column density of o-H2O N(o-H2O) < 2.5 x 10(13) cm(-2), or a fractional abundance x(o-H2O) < 1.3 x 10(-9), more than an order of magnitude lower than the SWAS upper limit on this source. The L1544 spectrum shows an absorption feature at a 5 sigma level from which we obtain the first value of the o-H2O column density ever measured in dark clouds: N(o-H2O) = (8 +/- 4) x 10(12) cm(-2). The corresponding fractional abundance is x(o-H2O) similar or equal to 5 x 10(-9) at radii > 7000 AU and similar or equal to 2 x 10(-10) toward the center. The radiative transfer analysis shows that this is consistent with a x(o-H2O) profile peaking at similar or equal to 10(-8), 0.1 pc away from the core center, where both freeze-out and photodissociation are negligible. Conclusions. Herschel has provided the first measurement of water vapor in dark regions. Column densities of o-H2O are low, but prestellar cores such as L1544 (with their high central densities, strong continuum, and large envelopes) appear to be very promising tools to finally shed light on the solid/vapor balance of water in molecular clouds and oxygen chemistry in the earliest stages of star formation. C1 [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Caselli, P.; Codella, C.; Jacq, T.] Ist Nazl Fis Nucl, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Keto, E.; Melnick, G.; van Kempen, T. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pagani, L.; Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [Pagani, L.; Encrenaz, P.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Aikawa, Y.] Kobe Univ, Dept Earth & Planetary Sci, Nada Ku, Kobe, Hyogo 6578501, Japan. [Yildiz, U. A.; van Dishoeck, E. F.; Hogerheijde, M. R.; Kristensen, L. E.; Visser, R.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [van der Tak, F. F. S.; de Graauw, Th.; Helmich, F.; Jackson, B.; Kester, D.; Laauwen, W.; Luinge, W.; Marseille, M.; Risacher, C.; Shipman, R.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [van der Tak, F. F. S.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Tafalla, M.; Bachiller, R.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Bergin, E. A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Nisini, B.; Giannini, T.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [van Dishoeck, E. F.; Herczeg, G. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Benz, A. O.; Bruderer, S.; Wampfler, S. F.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.] CNRS INSU, UMR 5804, F-33271 Floirac, France. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Bjerkeli, P.; Liseau, R.; Olberg, M.] Chalmers, Dept Radio & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Benedettini, M.; di Giorgio, A. M.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] CSIC INTA, Ctr Astrobiol, Dept Astrofis, Madrid 28850, Spain. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Fuente, A.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Gaier, T.; Javadi, H.; Pearson, J. C.; Siegel, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Lis, D.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [McCoey, C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Neufeld, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Parise, B.; Wyrowski, F.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Santiago-Garcia, J.] Inst Radioastron Milimetr IRAM, Granada 18012, Spain. [Megej, A.] ETH, Microwave Lab, CH-8092 Zurich, Switzerland. RP Caselli, P (reprint author), Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. EM p.caselli@leeds.ac.uk RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Jorgensen, Jes Kristian/L-7936-2014; Wampfler, Susanne/D-2270-2015; Fuente, Asuncion/G-1468-2016; OI Giannini, Teresa/0000-0002-0224-096X; Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Jorgensen, Jes Kristian/0000-0001-9133-8047; Wampfler, Susanne/0000-0002-3151-7657; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118; Codella, Claudio/0000-0003-1514-3074; , Brunella Nisini/0000-0002-9190-0113 NR 39 TC 28 Z9 28 U1 1 U2 7 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L29 DI 10.1051/0004-6361/201015097 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900029 ER PT J AU Ceccarelli, C Bacmann, A Boogert, A Caux, E Dominik, C Lefloch, B Lis, D Schilke, P van der Tak, F Caselli, P Cernicharo, J Codella, C Comito, C Fuente, A Baudry, A Bell, T Benedettini, M Bergin, EA Blake, GA Bottinelli, S Cabrit, S Castets, A Coutens, A Crimier, N Demyk, K Encrenaz, P Falgarone, E Gerin, M Goldsmith, PF Helmich, F Hennebelle, P Henning, T Herbst, E Hily-Blant, P Jacq, T Kahane, C Kama, M Klotz, A Langer, W Lord, S Lorenzani, A Maret, S Melnick, G Neufeld, D Nisini, B Pacheco, S Pagani, L Parise, B Pearson, J Phillips, T Salez, M Saraceno, P Schuster, K Tielens, X van der Wiel, MHD Vastel, C Viti, S Wakelam, V Walters, A Wyrowski, F Yorke, H Liseau, R Olberg, M Szczerba, R Benz, AO Melchior, M AF Ceccarelli, C. Bacmann, A. Boogert, A. Caux, E. Dominik, C. Lefloch, B. Lis, D. Schilke, P. van der Tak, F. Caselli, P. Cernicharo, J. Codella, C. Comito, C. Fuente, A. Baudry, A. Bell, T. Benedettini, M. Bergin, E. A. Blake, G. A. Bottinelli, S. Cabrit, S. Castets, A. Coutens, A. Crimier, N. Demyk, K. Encrenaz, P. Falgarone, E. Gerin, M. Goldsmith, P. F. Helmich, F. Hennebelle, P. Henning, T. Herbst, E. Hily-Blant, P. Jacq, T. Kahane, C. Kama, M. Klotz, A. Langer, W. Lord, S. Lorenzani, A. Maret, S. Melnick, G. Neufeld, D. Nisini, B. Pacheco, S. Pagani, L. Parise, B. Pearson, J. Phillips, T. Salez, M. Saraceno, P. Schuster, K. Tielens, X. van der Wiel, M. H. D. Vastel, C. Viti, S. Wakelam, V. Walters, A. Wyrowski, F. Yorke, H. Liseau, R. Olberg, M. Szczerba, R. Benz, A. O. Melchior, M. TI Herschel spectral surveys of star- forming regions Overview of the 555-636 GHz range SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; stars: formation ID NGC 6334 I; PROTOSTELLAR SHOCK L1157-B1; MASSIVE YOUNG STARS; DEUTERATED FORMALDEHYDE; HOT CORE; SUBMILLIMETER; MILLIMETER; PROTOSTARS; WATER; I(N) AB High resolution line spectra of star-forming regions are mines of information: they provide unique clues to reconstruct the chemical, dynamical, and physical structure of the observed source. We present the first results from the Herschel key project " Chemical HErschel Surveys of Star forming regions", CHESS. We report and discuss observations towards five CHESS targets, one outflow shock spot and four protostars with luminosities bewteen 20 and 2 x 105 L similar to : L1157-B1, IRAS 16293-2422, OMC2-FIR4, AFGL 2591, and NGC 6334I. The observations were obtained with the heterodyne spectrometer HIFI on board Herschel, with a spectral resolution of 1 MHz. They cover the frequency range 555-636 GHz, a range largely unexplored before the launch of the Herschel satellite. A comparison of the five spectra highlights spectacular differences in the five sources, for example in the density of methanol lines, or the presence./absence of lines from S-bearing molecules or deuterated species. We discuss how these differences can be attributed to the different star-forming mass or evolutionary status. C1 [Ceccarelli, C.; Bacmann, A.; Lefloch, B.; Castets, A.; Crimier, N.; Hily-Blant, P.; Kahane, C.; Maret, S.; Pacheco, S.] Univ Grenoble 1, CNRS, UMR 5571, Lab Astrophys Grenoble, Grenoble, France. [Ceccarelli, C.; Bacmann, A.; Baudry, A.; Castets, A.; Jacq, T.; Wakelam, V.] Univ Bordeaux, Lab Astrophys Bordeaux, Floirac, France. [Ceccarelli, C.; Bacmann, A.; Baudry, A.; Castets, A.; Jacq, T.; Wakelam, V.] CNRS INSU, UMR 5804, Floirac, France. [Boogert, A.; Lord, S.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Caux, E.; Bottinelli, S.; Coutens, A.; Demyk, K.; Klotz, A.; Vastel, C.; Walters, A.] Univ Toulouse 3, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse, France. [Caux, E.; Bottinelli, S.; Coutens, A.; Demyk, K.; Klotz, A.; Vastel, C.; Walters, A.] CNRS INSU, UMR 5187, Toulouse, France. [Dominik, C.; Kama, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6525 ED Nijmegen, Netherlands. [Schilke, P.; Comito, C.; Parise, B.; Wyrowski, F.] Max Planck Inst Radioastron, D-5300 Bonn, Germany. [Schilke, P.] Univ Cologne, Inst Phys 1, D-5000 Cologne, Germany. [van der Tak, F.; Helmich, F.; van der Wiel, M. H. D.; Olberg, M.] SRON Netherlands Inst Space Res, Groningen, Netherlands. [van der Tak, F.; van der Wiel, M. H. D.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands. [Caselli, P.; Benedettini, M.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Rome, Italy. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds, W Yorkshire, England. [Cernicharo, J.; Crimier, N.] CSIC INTA, Ctr Astrobiol, Madrid, Spain. [Codella, C.; Lorenzani, A.] INAF Osservatorio Astrofis Arcetri, Florence, Italy. [Fuente, A.] IGN Observ Astron Nacl, Alcala De Henares, Spain. [Bergin, E. A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Cabrit, S.; Encrenaz, P.; Falgarone, E.; Gerin, M.; Hennebelle, P.; Pagani, L.; Salez, M.] UCP, UPMC, Lab Etud Rayonnement & Mat Astrophys, UMR 8112,CNRS INSU,OP,ENS, Paris, France. [Goldsmith, P. F.; Langer, W.; Pearson, J.; Yorke, H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Herbst, E.] Ohio State Univ, Columbus, OH 43210 USA. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neufeld, D.] Johns Hopkins Univ, Baltimore, MD USA. [Nisini, B.] INAF Osservatorio Astronom Roma, Monte Porzio Catone, Italy. [Schuster, K.] Inst RadioAstron Millimetr, Grenoble, France. [Tielens, X.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Viti, S.] UCL, Dept Phys & Astron, London, England. [Liseau, R.; Olberg, M.] Stockholm Univ, Dept Astron, Chalmers Univ Technol, S-10691 Stockholm, Sweden. [Szczerba, R.] Nicholas Copernicus Astron Ctr, Torun, Poland. [Benz, A. O.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. RP Ceccarelli, C (reprint author), Univ Grenoble 1, CNRS, UMR 5571, Lab Astrophys Grenoble, Grenoble, France. EM cecilia.ceccarelli@obs.ujf-grenoble.fr RI van der Wiel, Matthijs/M-4531-2014; Coutens, Audrey/M-4533-2014; Fuente, Asuncion/G-1468-2016; Goldsmith, Paul/H-3159-2016; OI Maret, Sebastien/0000-0003-1104-4554; van der Wiel, Matthijs/0000-0002-4325-3011; Coutens, Audrey/0000-0003-1805-3920; Fuente, Asuncion/0000-0001-6317-6343; Lorenzani, Andrea/0000-0002-4685-3434; Wakelam, Valentine/0000-0001-9676-2605; Kama, Mihkel/0000-0003-0065-7267; Codella, Claudio/0000-0003-1514-3074; , Brunella Nisini/0000-0002-9190-0113 FU Swedish National Space Board, Stockholm University -Stockholm Observatory FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France abd the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiolog a (CSIC-INTA). Sweden: Chalmers University of Technology -MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University -Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. We thank many funding agencies for financial NR 34 TC 63 Z9 63 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L22 DI 10.1051/0004-6361/201015081 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900022 ER PT J AU Chavarria, L Herpin, F Jacq, T Braine, J Bontemps, S Baudry, A Marseille, M van der Tak, F Pietropaoli, B Wyrowski, F Shipman, R Frieswijk, W van Dishoeck, EF Cernicharo, J Bachiller, R Benedettini, M Benz, AO Bergin, E Bjerkeli, P Blake, GA Bruderer, S Caselli, P Codella, C Daniel, F di Giorgio, AM Dominik, C Doty, SD Encrenaz, P Fich, M Fuente, A Giannini, T Goicoechea, JR de Graauw, T Hartogh, P Helmich, F Herczeg, GJ Hogerheijde, MR Johnstone, D Jorgensen, JK Kristensen, LE Larsson, B Lis, D Liseau, R McCoey, C Melnick, G Nisini, B Olberg, M Parise, B Pearson, JC Plume, R Risacher, C Santiago-Garcia, J Saraceno, P Stutzki, J Szczerba, R Tafalla, M Tielens, A van Kempen, TA Visser, R Wampfler, SF Willem, J Yildiz, UA AF Chavarria, L. Herpin, F. Jacq, T. Braine, J. Bontemps, S. Baudry, A. Marseille, M. van der Tak, F. Pietropaoli, B. Wyrowski, F. Shipman, R. Frieswijk, W. van Dishoeck, E. F. Cernicharo, J. Bachiller, R. Benedettini, M. Benz, A. O. Bergin, E. Bjerkeli, P. Blake, G. A. Bruderer, S. Caselli, P. Codella, C. Daniel, F. di Giorgio, A. M. Dominik, C. Doty, S. D. Encrenaz, P. Fich, M. Fuente, A. Giannini, T. Goicoechea, J. R. de Graauw, Th. Hartogh, P. Helmich, F. Herczeg, G. J. Hogerheijde, M. R. Johnstone, D. Jorgensen, J. K. Kristensen, L. E. Larsson, B. Lis, D. Liseau, R. McCoey, C. Melnick, G. Nisini, B. Olberg, M. Parise, B. Pearson, J. C. Plume, R. Risacher, C. Santiago-Garcia, J. Saraceno, P. Stutzki, J. Szczerba, R. Tafalla, M. Tielens, A. van Kempen, T. A. Visser, R. Wampfler, S. F. Willem, J. Yildiz, U. A. TI Water in massive star-forming regions: HIFI observations of W3 IRS5 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; stars: massive; ISM: molecules; ISM: abundances; dust, extinction; radio lines: ISM ID RADIATIVE-TRANSFER; ABUNDANCES; ENVELOPES; RATIOS; SPECTROSCOPY; PROTOSTARS; TRAPEZIUM; CONTINUUM; TRACERS; MODELS AB We present Herschel observations of the water molecule in the massive star-forming region W3 IRS5. The o-(H2O)-O-17 1(10)-1(01), p-(H2O)-O-18 1(11)-0(00), p-H2O 2(02)-1(11), p-H2O 1(11)-0(00), o-H2O 2(21)-2(12), and o-H2O 2(12)-1(01) lines, covering a frequency range from 552 up to 1669 GHz, have been detected at high spectral resolution with HIFI. The water lines in W3 IRS5 show well-defined high-velocity wings that indicate a clear contribution by outflows. Moreover, the systematically blue-shifted absorption in the H2O lines suggests expansion, presumably driven by the outflow. No infall signatures are detected. The p-H2O 1(11)-0(00) and o-H2O 2(12)-1(01) lines show absorption from the cold material (T similar to 10 K) in which the high-mass protostellar envelope is embedded. One-dimensional radiative transfer models are used to estimate water abundances and to further study the kinematics of the region. We show that the emission in the rare isotopologues comes directly from the inner parts of the envelope (T greater than or similar to 100 K) where water ices in the dust mantles evaporate and the gas-phase abundance increases. The resulting jump in the water abundance (with a constant inner abundance of 10(-4)) is needed to reproduce the o-(H2O)-O-17 1(10)-1(01) and p-(H2O)-O-18 1(11)-0(00) spectra in our models. We estimate water abundances of 10(-8) to 10(-9) in the outer parts of the envelope (T less than or similar to 100 K). The possibility of two protostellar objects contributing to the emission is discussed. C1 [Chavarria, L.; Herpin, F.; Jacq, T.; Braine, J.; Bontemps, S.; Baudry, A.; Pietropaoli, B.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Chavarria, L.; Herpin, F.; Jacq, T.; Braine, J.; Bontemps, S.; Baudry, A.; Pietropaoli, B.] CNRS INSU, UMR 5804, Floirac, France. [Marseille, M.; van der Tak, F.; Shipman, R.; Frieswijk, W.; de Graauw, Th.; Helmich, F.; Willem, J.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [van der Tak, F.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Pietropaoli, B.] Ecole Mines, F-44300 Nantes, France. [Wyrowski, F.; Parise, B.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [van Dishoeck, E. F.; Hogerheijde, M. R.; Kristensen, L. E.; Tielens, A.; Visser, R.; Yildiz, U. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] CSIC INTA, Dept Astrofis, Ctr Astrobiol, Madrid 28850, Spain. [Bachiller, R.; Tafalla, M.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Benedettini, M.; di Giorgio, A. M.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Benz, A. O.; Bruderer, S.; Wampfler, S. F.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Bergin, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bjerkeli, P.; Liseau, R.; Olberg, M.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Caselli, P.; Codella, C.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [Encrenaz, P.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Fuente, A.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Giannini, T.; Nisini, B.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Hartogh, P.] MPI Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V9E 2E7, Canada. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Lis, D.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [McCoey, C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Melnick, G.; van Kempen, T. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Santiago-Garcia, J.] IRAM, E-18012 Granada, Spain. [Stutzki, J.] Univ Cologne, Inst Phys 1, KOSMA, D-50937 Cologne, Germany. [Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. RP Chavarria, L (reprint author), Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. EM luisagustinchavarria@gmail.com RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Wampfler, Susanne/D-2270-2015; Fuente, Asuncion/G-1468-2016; OI Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Wampfler, Susanne/0000-0002-3151-7657; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118; Codella, Claudio/0000-0003-1514-3074; Giannini, Teresa/0000-0002-0224-096X; , Brunella Nisini/0000-0002-9190-0113 FU French Space Agency CNES FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada, and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands, and with major contributions from Germany, France, and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. HIPE is a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS and SPIRE consortia. We also thank the French Space Agency CNES for financial support. NR 31 TC 36 Z9 36 U1 1 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L37 DI 10.1051/0004-6361/201015113 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900037 ER PT J AU Comito, C Schilke, P Rolffs, R Lis, DC Belloche, A Bergin, EA Phillips, TG Bell, TA Crockett, NR Wang, S Blake, GA Caux, E Ceccarelli, C Cernicharo, J Daniel, F Dubernet, ML Emprechtinger, M Encrenaz, P Gerin, M Giesen, TF Goicoechea, JR Goldsmith, PF Gupta, H Herbst, E Joblin, C Johnstone, D Langer, WD Latter, WD Lord, SD Maret, S Martin, PG Melnick, GJ Menten, KM Morris, P Muller, HSP Murphy, JA Neufeld, DA Ossenkopf, V Pearson, JC Perault, M Plume, R Qin, SL Schlemmer, S Stutzki, J Trappe, N van der Tak, FFS Vastel, C Yorke, HW Yu, S Olberg, M Szczerba, R Larsson, B Liseau, R Lin, RH Samoska, LA Schlecht, E AF Comito, C. Schilke, P. Rolffs, R. Lis, D. C. Belloche, A. Bergin, E. A. Phillips, T. G. Bell, T. A. Crockett, N. R. Wang, S. Blake, G. A. Caux, E. Ceccarelli, C. Cernicharo, J. Daniel, F. Dubernet, M. -L. Emprechtinger, M. Encrenaz, P. Gerin, M. Giesen, T. F. Goicoechea, J. R. Goldsmith, P. F. Gupta, H. Herbst, E. Joblin, C. Johnstone, D. Langer, W. D. Latter, W. D. Lord, S. D. Maret, S. Martin, P. G. Melnick, G. J. Menten, K. M. Morris, P. Mueller, H. S. P. Murphy, J. A. Neufeld, D. A. Ossenkopf, V. Pearson, J. C. Perault, M. Plume, R. Qin, S. -L. Schlemmer, S. Stutzki, J. Trappe, N. van der Tak, F. F. S. Vastel, C. Yorke, H. W. Yu, S. Olberg, M. Szczerba, R. Larsson, B. Liseau, R. Lin, R. H. Samoska, L. A. Schlecht, E. TI Herschel observations of deuterated water towards Sgr B2(M) SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: molecules; molecular processes; line: formation ID LINE OBSERVATIONS; HOT CORES; SAGITTARIUS-B2; SUBMILLIMETER; EXCITATION; ASTRONOMY; VAPOR; BAND AB Observations of HDO are an important complement for studies of water, because they give strong constraints on the formation processes - grain surfaces versus energetic process in the gas phase, e. g. in shocks. The HIFI observations of multiple transitions of HDO in Sgr B2(M) presented here allow the determination of the HDO abundance throughout the envelope, which has not been possible before with ground-based observations only. The abundance structure has been modeled with the spherical Monte Carlo radiative transfer code RATRAN, which also takes radiative pumping by continuum emission from dust into account. The modeling reveals that the abundance of HDO rises steeply with temperature from a low abundance (2.5 x 10(-11)) in the outer envelope at temperatures below 100 K through a medium abundance (1.5 x 10(-9)) in the inner envelope/outer core at temperatures between 100 and 200 K, and finally a high abundance (3.5 x 10(-9)) at temperatures above 200 K in the hot core. C1 [Comito, C.; Schilke, P.; Rolffs, R.; Belloche, A.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Schilke, P.; Rolffs, R.; Giesen, T. F.; Mueller, H. S. P.; Ossenkopf, V.; Qin, S. -L.; Schlemmer, S.; Stutzki, J.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Lis, D. C.; Phillips, T. G.; Bell, T. A.; Blake, G. A.; Emprechtinger, M.] CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA. [Bergin, E. A.; Crockett, N. R.; Wang, S.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Caux, E.; Joblin, C.; Vastel, C.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.; Joblin, C.; Vastel, C.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Ceccarelli, C.; Maret, S.] Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Madrid, Spain. [Daniel, F.; Encrenaz, P.; Gerin, M.; Perault, M.] Observ Paris, LERMA, CNRS UMR8112, F-75231 Paris 05, France. [Daniel, F.; Encrenaz, P.; Gerin, M.; Perault, M.] Ecole Normale Super, F-75231 Paris 05, France. [Dubernet, M. -L.] Univ Paris 06, LPMAA, UMR7092, Paris, France. [Dubernet, M. -L.] Observ Paris, LUTH, UMR8102, Meudon, France. [Goldsmith, P. F.; Gupta, H.; Langer, W. D.; Pearson, J. C.; Yorke, H. W.; Yu, S.; Lin, R. H.; Samoska, L. A.; Schlecht, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Latter, W. D.; Lord, S. D.; Morris, P.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murphy, J. A.; Trappe, N.] Natl Univ Ireland Maynooth, Maynooth, Kildare, Ireland. [Neufeld, D. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Ossenkopf, V.; van der Tak, F. F. S.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Olberg, M.; Liseau, R.] Chalmers, S-41296 Gothenburg, Sweden. [Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. RP Comito, C (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM ccomito@mpifr.de RI Giesen, Thomas /B-9476-2015; Schlemmer, Stephan/E-2903-2015; Trappe, Neil/C-9014-2016; Yu, Shanshan/D-8733-2016; Goldsmith, Paul/H-3159-2016 OI Mueller, Holger/0000-0002-0183-8927; Maret, Sebastien/0000-0003-1104-4554; Giesen, Thomas /0000-0002-2401-0049; Schlemmer, Stephan/0000-0002-1421-7281; Trappe, Neil/0000-0003-2527-9821; FU NASA through JPL/Caltech; NSF [AST-0540882] FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri- INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronifimico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. CSO is supported by the NSF, award AST-0540882. NR 24 TC 7 Z9 7 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L38 DI 10.1051/0004-6361/201015121 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900038 ER PT J AU Covino, S Campana, S Conciatore, ML D'Elia, V Palazzi, E Thone, CC Vergani, SD Wiersema, K Brusasca, M Cucchiara, A Cobb, BE Fernandez-Soto, A Kann, DA Malesani, D Tanvir, NR Antonelli, LA Bremer, M Castro-Tirado, AJ Postigo, AD Molinari, E Nicastro, L Stefanon, M Testa, V Tosti, G Vitali, F Amati, L Chapman, R Conconi, P Cutispoto, G Fynbo, JPU Goldoni, P Henriksen, C Horne, KD Malaspina, G Meurs, EJA Pian, E Stella, L Tagliaferri, G Ward, P Zerbi, FM AF Covino, S. Campana, S. Conciatore, M. L. D'Elia, V. Palazzi, E. Thoene, C. C. Vergani, S. D. Wiersema, K. Brusasca, M. Cucchiara, A. Cobb, B. E. Fernandez-Soto, A. Kann, D. A. Malesani, D. Tanvir, N. R. Antonelli, L. A. Bremer, M. Castro-Tirado, A. J. Postigo, A. de Ugarte Molinari, E. Nicastro, L. Stefanon, M. Testa, V. Tosti, G. Vitali, F. Amati, L. Chapman, R. Conconi, P. Cutispoto, G. Fynbo, J. P. U. Goldoni, P. Henriksen, C. Horne, K. D. Malaspina, G. Meurs, E. J. A. Pian, E. Stella, L. Tagliaferri, G. Ward, P. Zerbi, F. M. TI Challenging gamma-ray burst models through the broadband dataset of GRB060908 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma-ray burst: individual: GRB 060908; gamma-ray burst: general; radiation mechanisms: non-thermal ID SWIFT XRT DATA; AFTERGLOW LIGHT CURVES; EARLY OPTICAL AFTERGLOWS; REVERSE SHOCK EMISSION; X-RAY; COMPREHENSIVE ANALYSIS; MULTIWAVELENGTH ANALYSIS; PARTICLE-ACCELERATION; RELATIVISTIC JETS; CANNONBALL MODEL AB Context. Multiwavelength observations of gamma-ray burst prompt and afterglow emission are a key tool to separate the various possible emission processes and scenarios proposed to interpret the complex gamma-ray burst phenomenology. Aims. We collected a large dataset on GRB060908 in order to carry out a comprehensive analysis of the prompt emission as well as the early and late afterglow. Methods. Data from Swift-BAT, -XRT and -UVOT together with data from a number of different ground-based optical/near-infrared and millimeter telescopes allowed us to follow the afterglow evolution after about a minute from the high-energy event down to the host galaxy limit. We discuss the physical parameters required to model these emissions. Results. The prompt emission of GRB060908 was characterised by two main periods of activity, spaced by a few seconds of low intensity, with a tight correlation between activity and spectral hardness. Observations of the afterglow began less than one minute after the high-energy event, when it was already in a decaying phase, and it was characterised by a rather flat optical/near-infrared spectrum which can be interpreted as due to a hard energy-distribution of the emitting electrons. On the other hand, the X-ray spectrum of the afterglow could be fit by a rather soft electron distribution. Conclusions. GRB060908 is a good example of a gamma-ray burst with a rich multi-wavelength set of observations. The availability of this dataset, built thanks to the joint efforts of many different teams, allowed us to carry out stringent tests for various interpretative scenarios, showing that a satisfactorily modelling of this event is challenging. In the future, similar efforts will enable us to obtain optical/near-infrared coverage comparable in quality and quantity to the X-ray data for more events, therefore opening new avenues to progress gamma-ray burst research. C1 [Covino, S.; Campana, S.; Thoene, C. C.; Brusasca, M.; Postigo, A. de Ugarte; Conconi, P.; Malaspina, G.; Tagliaferri, G.; Zerbi, F. M.] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. [Campana, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [D'Elia, V.; Antonelli, L. A.; Testa, V.; Vitali, F.; Stella, L.] Osserv Astron Roma, INAF, I-00040 Rome, Italy. [Palazzi, E.; Nicastro, L.; Amati, L.] Ist Astrofis Spaziale & Fis Cosm Bologna, INAF, I-40129 Bologna, Italy. [Vergani, S. D.; Goldoni, P.] APC, Lab Astroparticule & Cosmol, UMR 7164, F-75231 Paris 05, France. [Vergani, S. D.; Goldoni, P.] CEA Saclay, DSM, Serv Astrophys, DAPNIA, F-91191 Gif Sur Yvette, France. [Wiersema, K.; Tanvir, N. R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Cucchiara, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Cobb, B. E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Fernandez-Soto, A.] CSIC UC, Inst Fis Cantabria, Santander 39005, Spain. [Kann, D. A.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Malesani, D.; Fynbo, J. P. U.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Bremer, M.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Castro-Tirado, A. J.] Inst Astrofis Andalucia, E-18080 Granada, Spain. [Molinari, E.] INAF TNG Fdn Galileo Galilei, Brena Baja 38712, TF, Spain. [Stefanon, M.] Univ Valencia, Astron Observ, Valencia 46980, Spain. [Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Tosti, G.] Univ Perugia, Osservatorio Astron, I-06123 Perugia, Italy. [Chapman, R.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Chapman, R.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland. [Cutispoto, G.] Catania Astrophys Observ, INAF, I-95123 Catania, Italy. [Horne, K. D.] Univ St Andrews, SUPA Phys & Astron, St Andrews KY 9SS, Fife, Scotland. [Meurs, E. J. A.; Ward, P.] Dunsink Observ, DIAS, Dublin 15, Ireland. [Pian, E.] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy. [Pian, E.] Scuola Normale Super Pisa, I-56126 Pisa, Italy. RP Covino, S (reprint author), Osserv Astron Brera, INAF, Via Emilio Bianchi 46, I-23807 Merate, LC, Italy. EM stefano.covino@brera.inaf.it RI Tosti, Gino/E-9976-2013; Fynbo, Johan/L-8496-2014; Nicastro, Luciano/F-5866-2015; Palazzi, Eliana/N-4746-2015; Amati, Lorenzo/N-5586-2015; Stefanon, Mauro/F-8708-2016; Fernandez-Soto, Alberto/A-2443-2009; OI Zerbi, Filippo Maria/0000-0002-9996-973X; Campana, Sergio/0000-0001-6278-1576; Fynbo, Johan/0000-0002-8149-8298; Nicastro, Luciano/0000-0001-8534-6788; Amati, Lorenzo/0000-0001-5355-7388; Stefanon, Mauro/0000-0001-7768-5309; Fernandez-Soto, Alberto/0000-0002-5732-3121; Palazzi, Eliana/0000-0002-8691-7666; Molinari, Emilio/0000-0002-1742-7735; Testa, Vincenzo/0000-0003-1033-1340; Pian, Elena/0000-0001-8646-4858; Vitali, Fabrizio/0000-0001-8332-4227; D'Elia, Valerio/0000-0002-7320-5862; Castro-Tirado, A. J./0000-0003-2999-3563; Thone, Christina/0000-0002-7978-7648; de Ugarte Postigo, Antonio/0000-0001-7717-5085; Covino, Stefano/0000-0001-9078-5507; Tagliaferri, Gianpiero/0000-0003-0121-0723 FU NSF [AST 0707627]; Spanish MICINN [AYA2006-14056]; Generalitat Valenciana [2008/132] FX The SMARTS project is supported by NSF-AST 0707627. S.C. thanks Paolo D'Avanzo, Arnon Dar, Yizhong Fan, Dino Fugazza, Gabriele Ghisellini, Cristiano Guidorzi, Ruben Salvaterra and Zhiping Zin for many useful discussions. A.F.S. acknowledges support from the Spanish MICINN projects AYA2006-14056, Consolider-Ingenio 2007-32022, and from the Generalitat Valenciana project Prometeo 2008/132. We also acknowledge the use of data obtained with the Danish 1.5 m telescope as part of a program led by Jens Hjorth. NR 122 TC 17 Z9 18 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR A53 DI 10.1051/0004-6361/201014994 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900114 ER PT J AU Crockett, NR Bergin, EA Wang, S Lis, DC Bell, TA Blake, GA Boogert, A Bumble, B Cabrit, S Caux, E Ceccarelli, C Cernicharo, J Daniel, F Daniel, F Dubernet, ML Emprechtinger, M Encrenaz, P Falgarone, E Gerin, M Giesen, TF Goicoechea, JR Goldsmith, PF Gupta, H Gusten, R Hartogh, P Helmich, F Herbst, E Honingh, N Joblin, C Johnstone, D Karpov, A Kawamura, JH Kooi, J Krieg, JM Langer, WD Latter, WD Lord, SD Maret, S Martin, PG Melnick, GJ Menten, KM Morris, P Muller, HSP Murphy, JA Neufeld, DA Ossenkopf, V Pearson, JC Perault, M Phillips, TG Plume, R Qin, SL Roelfsema, P Schieder, R Schilke, P Schlemmer, S Stutzki, J van der Tak, FFS Tielens, A Trappe, N Vastel, C Yorke, HW Yu, S Zmuidzinas, J AF Crockett, N. R. Bergin, E. A. Wang, S. Lis, D. C. Bell, T. A. Blake, G. A. Boogert, A. Bumble, B. Cabrit, S. Caux, E. Ceccarelli, C. Cernicharo, J. Daniel, F. Daniel, F. Dubernet, M. -L. Emprechtinger, M. Encrenaz, P. Falgarone, E. Gerin, M. Giesen, T. F. Goicoechea, J. R. Goldsmith, P. F. Gupta, H. Guesten, R. Hartogh, P. Helmich, F. Herbst, E. Honingh, N. Joblin, C. Johnstone, D. Karpov, A. Kawamura, J. H. Kooi, J. Krieg, J. -M. Langer, W. D. Latter, W. D. Lord, S. D. Maret, S. Martin, P. G. Melnick, G. J. Menten, K. M. Morris, P. Mueller, H. S. P. Murphy, J. A. Neufeld, D. A. Ossenkopf, V. Pearson, J. C. Perault, M. Phillips, T. G. Plume, R. Qin, S. -L. Roelfsema, P. Schieder, R. Schilke, P. Schlemmer, S. Stutzki, J. van der Tak, F. F. S. Tielens, A. Trappe, N. Vastel, C. Yorke, H. W. Yu, S. Zmuidzinas, J. TI Herschel observations of EXtra-Ordinary Sources (HEXOS): The Terahertz spectrum of Orion KL seen at high spectral resolution SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; ISM: general; ISM: clouds; ISM: molecules; submillimeter: ISM ID MOLECULAR LINE SURVEY; APERTURE SYNTHESIS; COLOGNE DATABASE; SUBMILLIMETER; SPECTROSCOPY; MILLIMETER; NEBULA; CLOUDS; CDMS; HIFI AB We present the first high spectral resolution observations of Orion KL in the frequency ranges 1573.4-1702.8 GHz (band 6b) and 1788.4-1906.8 GHz (band 7b) obtained using the HIFI instrument on board the Herschel Space Observatory. We characterize the main emission lines found in the spectrum, which primarily arise from a range of components associated with Orion KL including the hot core, but also see widespread emission from components associated with molecular outflows traced by H2O, SO2, and OH. We find that the density of observed emission lines is significantly diminished in these bands compared to lower frequency Herschel/HIFI bands. C1 [Crockett, N. R.; Bergin, E. A.; Wang, S.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Lis, D. C.; Bell, T. A.; Blake, G. A.; Emprechtinger, M.; Karpov, A.; Kooi, J.; Phillips, T. G.; Zmuidzinas, J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Neufeld, D. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Caux, E.; Joblin, C.; Vastel, C.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.; Joblin, C.; Vastel, C.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Ceccarelli, C.; Maret, S.] Lab Astrophys Observ Grenoble, F-38041 Grenoble 9, France. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Madrid 28850, Spain. [Daniel, F.; Guesten, R.; Menten, K. M.; Schilke, P.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Daniel, F.; Encrenaz, P.; Gerin, M.; Krieg, J. -M.; Perault, M.] Observ Paris, UMR8112, CNRS, LERMA, F-75231 Paris 05, France. [Daniel, F.; Encrenaz, P.; Gerin, M.; Krieg, J. -M.; Perault, M.] Ecole Normale Super, F-75231 Paris 05, France. [Dubernet, M. -L.] Univ Paris 06, LPMAA, UMR7092, Paris, France. [Dubernet, M. -L.] Observ Paris, UMR8102, LUTH, Meudon, France. [Giesen, T. F.; Honingh, N.; Mueller, H. S. P.; Ossenkopf, V.; Qin, S. -L.; Schieder, R.; Schilke, P.; Schlemmer, S.; Stutzki, J.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Bumble, B.; Goldsmith, P. F.; Gupta, H.; Kawamura, J. H.; Langer, W. D.; Pearson, J. C.; Yorke, H. W.; Yu, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Boogert, A.; Latter, W. D.; Lord, S. D.; Morris, P.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murphy, J. A.; Trappe, N.] Natl Univ Ireland Maynooth, Maynooth, Kildare, Ireland. [Helmich, F.; Ossenkopf, V.; Roelfsema, P.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Plume, R.; van der Tak, F. F. S.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Hartogh, P.] MPI Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Tielens, A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Cabrit, S.] Observ Paris, CNRS, UMR8112, F-75014 Paris, France. [Cabrit, S.] LERMA, F-75014 Paris, France. [Falgarone, E.] Observ Paris, UMR8112, CNRS, LERMA, F-75231 Paris 05, France. [Falgarone, E.] Ecole Normale Super, F-75231 Paris 05, France. RP Crockett, NR (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM ncrocket@umich.edu RI Giesen, Thomas /B-9476-2015; Schlemmer, Stephan/E-2903-2015; Trappe, Neil/C-9014-2016; Yu, Shanshan/D-8733-2016; Goldsmith, Paul/H-3159-2016 OI Mueller, Holger/0000-0002-0183-8927; Giesen, Thomas /0000-0002-2401-0049; Schlemmer, Stephan/0000-0002-1421-7281; Maret, Sebastien/0000-0003-1104-4554; Trappe, Neil/0000-0003-2527-9821; FU NASA; NSF [AST0540882] FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astron mico Nacional (IGN), Centro de Astrobiolog a (CSIC-INTA). Sweden: Chalmers University of Technology -MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University -Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. CSO is supported by the NSF, award AST0540882. NR 20 TC 17 Z9 17 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L21 DI 10.1051/0004-6361/201015116 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900021 ER PT J AU Decin, L Justtanont, K De Beck, E Lombaert, R de Koter, A Waters, LBFM Marston, AP Teyssier, D Schoier, FL Bujarrabal, V Alcolea, J Cernicharo, J Dominik, C Melnick, G Menten, K Neufeld, DA Olofsson, H Planesas, P Schmidt, M Szczerba, R de Graauw, T Helmich, F Roelfsema, P Dieleman, P Morris, P Gallego, JD Diez-Gonzalez, MC Caux, E AF Decin, L. Justtanont, K. De Beck, E. Lombaert, R. de Koter, A. Waters, L. B. F. M. Marston, A. P. Teyssier, D. Schoier, F. L. Bujarrabal, V. Alcolea, J. Cernicharo, J. Dominik, C. Melnick, G. Menten, K. Neufeld, D. A. Olofsson, H. Planesas, P. Schmidt, M. Szczerba, R. de Graauw, T. Helmich, F. Roelfsema, P. Dieleman, P. Morris, P. Gallego, J. D. Diez-Gonzalez, M. C. Caux, E. TI Water content and wind acceleration in the envelope around the oxygen-rich AGB star IK Tauri as seen by Herschel/HIFI SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE line: profiles; radiative transfer; instrumentation: spectrographs; stars: AGB and post-AGB; circumstellar matter; submillimeter: stars ID GIANT BRANCH STARS; MASS-LOSS HISTORY; CIRCUMSTELLAR ENVELOPES; EVOLVED STARS; ISOTOPIC ABUNDANCES; LINE EMISSION; CARBON STARS; W-HYA; CO; VAPOR AB During their asymptotic giant branch evolution, low-mass stars lose a significant fraction of their mass through an intense wind, enriching the interstellar medium with products of nucleosynthesis. We observed the nearby oxygen-rich asymptotic giant branch star IK Tau using the high-resolution HIFI spectrometer onboard Herschel. We report on the first detection of (H2O)-O-16 and the rarer isotopologues (H2O)-O-17 and (H2O)-O-18 in both the ortho and para states. We deduce a total water content (relative to molecular hydrogen) of 6.6 x 10(-5), and an ortho-to-para ratio of 3:1. These results are consistent with the formation of H2O in thermodynamical chemical equilibrium at photospheric temperatures, and does not require pulsationally induced non-equilibrium chemistry, vaporization of icy bodies or grain surface reactions. High-excitation lines of (CO)-C-12, (CO)-C-13, (SiO)-Si-28, (SiO)-Si-29, (SiO)-Si-30, HCN, and SO have also been detected. From the observed line widths, the acceleration region in the inner wind zone can be characterized, and we show that the wind acceleration is slower than hitherto anticipated. C1 [Decin, L.; De Beck, E.; Lombaert, R.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium. [Decin, L.; de Koter, A.; Waters, L. B. F. M.; Dominik, C.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1098 Amsterdam, Netherlands. [Justtanont, K.] Chalmers, Onsala Space Observ, Dept Radio & Spece Sci, S-43992 Onsala, Sweden. [de Koter, A.] Univ Utrecht, Astron Inst, NL-3584 CC Utrecht, Netherlands. [Marston, A. P.; Teyssier, D.] ESA, European Space Astron Ctr, Madrid, Spain. [Bujarrabal, V.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Alcolea, J.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Cernicharo, J.] INTA CSIC, CAB, Lab Mol Astrophys, Madrid 28850, Spain. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Menten, K.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Neufeld, D. A.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Olofsson, H.] Stockholm Univ, Dept Astron, AlbaNova Univ Ctr, S-10691 Stockholm, Sweden. [Schoier, F. L.; Olofsson, H.] Chalmers, Dept Radio & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Planesas, P.] Joint ALMA Observ, Santiago, Chile. [Schmidt, M.; Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. [de Graauw, T.] Joint ALMA Off, Santiago, Chile. [Helmich, F.; Roelfsema, P.; Dieleman, P.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Morris, P.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Gallego, J. D.; Diez-Gonzalez, M. C.] Ctr Astron Yebes, Observ Astron Nacl IGN, E-19080 Guadalajara, Spain. [Caux, E.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. RP Decin, L (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Heverlee, Belgium. EM Leen.Decin@ster.kuleuven.be; v.bujarrabal@oan.es RI Planesas, Pere/G-7950-2015; OI Planesas, Pere/0000-0002-7808-3040; De Beck, Elvire/0000-0002-7441-7189; /0000-0003-1689-9201 FU Flanders (FWO); Spanish MICINN [CSD2009-00038]; Polish MNiSW [N 203 393334]; MICINN [AYA2009-07304]; National Aeronautics and Space Administration FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri- INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA); Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. HCSS / HSpot / HIPE is a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS and SPIRE consortia. LD acknowledges financial support from the Fund for Scientific Research - Flanders (FWO). This work has been partially supported by the Spanish MICINN, program CONSOLIDER INGENIO 2010, grant ASTROMOL (CSD2009-00038). R.Sz. and M.Sch. acknowledge support from grant N 203 393334 from Polish MNiSW. J.C. thanks funding from MICINN, grant AYA2009-07304. This research was performed, in part, through a JPL contract funded by the National Aeronautics and Space Administration. NR 36 TC 31 Z9 31 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L4 DI 10.1051/0004-6361/201015069 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900004 ER PT J AU Guarcello, MG Damiani, F Micela, G Peres, G Prisinzano, L Sciortino, S AF Guarcello, M. G. Damiani, F. Micela, G. Peres, G. Prisinzano, L. Sciortino, S. TI Pre-main sequence stars with disks in the Eagle Nebula observed in scattered light SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; scattering; protoplanetary disks; circumstellar matter; stars: pre-main sequence; Hertzsprung-Russell and C-M diagrams ID SPECTRAL ENERGY-DISTRIBUTIONS; YOUNG STELLAR OBJECTS; T-TAURI STARS; ACCRETION DISKS; CIRCUMSTELLAR DISKS; SPATIAL-DISTRIBUTION; FORMING REGIONS; GALACTIC PLANE; MASSIVE STARS; GRAIN-GROWTH AB Context. NGC 6611 and its parental cloud, the Eagle Nebula (M 16), are well-studied star-forming regions, thanks to their large content of both OB stars and stars with disks and the observed ongoing star formation. In our previous studies of the Eagle Nebula, we identified 834 disk-bearing stars associated with the cloud, after detecting their excesses in NIR bands from J band to 8.0 mu m. Aims. In this paper, we study in detail the nature of a subsample of disk-bearing stars that show peculiar characteristics. They appear older than the other members in the V vs. V - I diagram, and/or they have one or more IRAC colors at pure photospheric values, despite showing NIR excesses, when optical and infrared colors are compared. Methods. We confirm the membership of these stars to M 16 by a spectroscopic analysis. The physical properties of these stars with disks are studied by comparing their spectral energy distributions (SEDs) with the SEDs predicted by models of T Tauri stars with disks and envelopes. Results. We show that the age of these stars estimated from the V vs. V - I diagram is unreliable since their V - I colors are altered by the light scattered by the disk into the line of sight. Only in a few cases their SEDs are compatible with models with excesses in V band caused by optical veiling. Candidate members with disks and photospheric IRAC colors are selected by the used NIR disk diagnostic, which is sensitive to moderate excesses, such as those produced by disks with low masses. In 1/3 of these cases, scattering of stellar flux by the disks can also be invoked. Conclusions. The photospheric light scattered by the disk grains into the line of sight can affect the derivation of physical parameters of Class II stars from photometric optical and NIR data. Besides, the disks diagnostic we defined are useful for selecting stars with disks, even those with moderate excesses or whose optical colors are altered by veiling or photospheric scattered light. C1 [Guarcello, M. G.; Damiani, F.; Micela, G.; Prisinzano, L.; Sciortino, S.] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy. [Guarcello, M. G.; Peres, G.] Univ Palermo, Dipartimento Sci Fis & Astron, I-90134 Palermo, Italy. RP Guarcello, MG (reprint author), Smithsonian Astrophys Observ, MS 3,60 Garden St, Cambridge, MA 02138 USA. EM mguarce@astropa.unipa.it OI Micela, Giuseppina/0000-0002-9900-4751; Prisinzano, Loredana/0000-0002-8893-2210; PERES, Giovanni/0000-0002-6033-8180; Damiani, Francesco/0000-0002-7065-3061 FU CONSTELLATION grant [YA 2007]; PRIN-INAF FX Support for this work has been provided by the CONSTELLATION grant YA 2007 and the contract PRIN-INAF (P. I.: Lanza). This work is based on data obtained as part of the UKIRT Infrared Deep Sky Survey, public data obtained with WFI@ESO, 2MASS Point Source Catalog and GLIMPSE survey with Spitzer/IRAC. The authors acknowledge M. Caramazza for her help in Spitzer data analysis. NR 34 TC 14 Z9 14 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR A18 DI 10.1051/0004-6361/201014237 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900079 ER PT J AU Gupta, H Rimmer, P Pearson, JC Yu, S Herbst, E Harada, N Bergin, EA Neufeld, DA Melnick, GJ Bachiller, R Baechtold, W Bell, TA Blake, GA Caux, E Ceccarelli, C Cernicharo, J Chattopadhyay, G Comito, C Cabrit, S Crockett, NR Daniel, F Falgarone, E Diez-Gonzalez, MC Dubernet, ML Erickson, N Emprechtinger, M Encrenaz, P Gerin, M Gill, JJ Giesen, TF Goicoechea, JR Goldsmith, PF Joblin, C Johnstone, D Langer, WD Larsson, B Latter, WB Lin, RH Lis, DC Liseau, R Lord, SD Maiwald, FW Maret, S Martin, PG Martin-Pintado, J Menten, KM Morris, P Muller, HSP Murphy, JA Nordh, LH Olberg, M Ossenkopf, V Pagani, L Perault, M Phillips, TG Plume, R Qin, SL Salez, M Samoska, LA Schilke, P Schlecht, E Schlemmer, S Szczerba, R Stutzki, J Trappe, N van der Tak, FFS Vastel, C Wang, S Yorke, HW Zmuidzinas, J Boogert, A Gusten, R Hartogh, P Honingh, N Karpov, A Kooi, J Krieg, JM Schieder, R Zaal, P AF Gupta, H. Rimmer, P. Pearson, J. C. Yu, S. Herbst, E. Harada, N. Bergin, E. A. Neufeld, D. A. Melnick, G. J. Bachiller, R. Baechtold, W. Bell, T. A. Blake, G. A. Caux, E. Ceccarelli, C. Cernicharo, J. Chattopadhyay, G. Comito, C. Cabrit, S. Crockett, N. R. Daniel, F. Falgarone, E. Diez-Gonzalez, M. C. Dubernet, M. -L. Erickson, N. Emprechtinger, M. Encrenaz, P. Gerin, M. Gill, J. J. Giesen, T. F. Goicoechea, J. R. Goldsmith, P. F. Joblin, C. Johnstone, D. Langer, W. D. Larsson, B. Latter, W. B. Lin, R. H. Lis, D. C. Liseau, R. Lord, S. D. Maiwald, F. W. Maret, S. Martin, P. G. Martin-Pintado, J. Menten, K. M. Morris, P. Mueller, H. S. P. Murphy, J. A. Nordh, L. H. Olberg, M. Ossenkopf, V. Pagani, L. Perault, M. Phillips, T. G. Plume, R. Qin, S. -L. Salez, M. Samoska, L. A. Schilke, P. Schlecht, E. Schlemmer, S. Szczerba, R. Stutzki, J. Trappe, N. van der Tak, F. F. S. Vastel, C. Wang, S. Yorke, H. W. Zmuidzinas, J. Boogert, A. Guesten, R. Hartogh, P. Honingh, N. Karpov, A. Kooi, J. Krieg, J. -M. Schieder, R. Zaal, P. TI Detection of OH+ and H2O+ towards Orion KL SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; molecular processes; line: identification; ISM: abundances; submillimeter: ISM; stars: winds; outflows ID LASER MAGNETIC-RESONANCE; HERSCHEL OBSERVATIONS; INTERSTELLAR H3O+; STAR-FORMATION; DIFFUSE CLOUDS; COMET-KOHOUTEK; NEBULA; LINE; REGION; SPECTROSCOPY AB We report observations of the reactive molecular ions OH+, H2O+, and H3O+ towards Orion KL with Herschel/HIFI. All three N = 1-0 fine-structure transitions of OH+ at 909, 971, and 1033 GHz and both fine-structure components of the doublet ortho-H2O+ 1(11)-0(00) transition at 1115 and 1139 GHz were detected; an upper limit was obtained for H3O+, OH+ and H2O+ are observed purely in absorption, showing a narrow component at the source velocity of 9 km s(-1), and a broad blueshifted absorption similar to that reported recently for HF and para-(H2O)-O-18, and attributed to the low velocity outflow of Orion KL. We estimate column densities of OH+ and H2O+ for the 9 km s(-1) component of 9 +/- 3x10(12) cm(-2) and 7 +/- 2x10(12) cm(-2), and those in the outflow of 1.9 +/- 0.7x10(13) cm(-2) and 1.0 +/- 0.3x10(13) cm(-2). Upper limits of 2.4x10(12) cm(-2) and 8.7x10(12) cm(-2) were derived for the column densities of ortho and para-H3O+ from transitions near 985 and 1657 GHz. The column densities of the three ions are up to an order of magnitude lower than those obtained from recent observations of W31C and W49N. The comparatively low column densities may be explained by a higher gas density despite the assumption of a very high ionization rate. C1 [Gupta, H.; Pearson, J. C.; Yu, S.; Chattopadhyay, G.; Gill, J. J.; Goldsmith, P. F.; Langer, W. D.; Lin, R. H.; Samoska, L. A.; Schlecht, E.; Yorke, H. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Rimmer, P.; Herbst, E.; Harada, N.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Rimmer, P.; Herbst, E.; Harada, N.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Rimmer, P.; Herbst, E.; Harada, N.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Bergin, E. A.; Crockett, N. R.; Wang, S.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Neufeld, D. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bachiller, R.; Diez-Gonzalez, M. C.] Observ Astron Nacl IGN, Ctr Astron Yebes, Guadalajara 19080, Spain. [Baechtold, W.] ETH, Microwave Lab, CH-8092 Zurich, Switzerland. [Bell, T. A.; Blake, G. A.; Emprechtinger, M.; Lis, D. C.; Zmuidzinas, J.; Boogert, A.; Kooi, J.] CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA. [Caux, E.; Joblin, C.; Vastel, C.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.; Joblin, C.; Vastel, C.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Ceccarelli, C.; Maret, S.] Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.; Martin-Pintado, J.; Krieg, J. -M.] Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Madrid 28850, Spain. [Comito, C.; Goicoechea, J. R.; Menten, K. M.; Schilke, P.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Cabrit, S.; Pagani, L.; Salez, M.] Observ Paris, LERMA, F-75014 Paris, France. [Cabrit, S.; Pagani, L.; Salez, M.] Observ Paris, CNRS, UMR8112, F-75014 Paris, France. [Daniel, F.; Falgarone, E.; Encrenaz, P.; Gerin, M.; Perault, M.] Observ Paris, CNRS UMR8112, LERMA, F-75231 Paris 05, France. [Dubernet, M. -L.] Univ Paris 06, UMR7092, LPMAA, Paris, France. [Dubernet, M. -L.] Observ Paris, UMR8102, LUTH, Meudon, France. [Erickson, N.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Giesen, T. F.; Mueller, H. S. P.; Ossenkopf, V.; Qin, S. -L.; Schilke, P.; Schlemmer, S.; Stutzki, J.; Schieder, R.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Larsson, B.; Liseau, R.; Nordh, L. H.; Olberg, M.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Johnstone, D.; Honingh, N.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Latter, W. B.; Lord, S. D.; Morris, P.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Liseau, R.; Olberg, M.] Chalmers, S-41296 Gothenburg, Sweden. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Murphy, J. A.; Trappe, N.] Natl Univ Ireland, Maynooth, Kildare, Ireland. [Ossenkopf, V.; van der Tak, F. F. S.; Zaal, P.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Hartogh, P.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. RP Gupta, H (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM hgupta@jpl.nasa.gov RI Goldsmith, Paul/H-3159-2016; Martin-Pintado, Jesus/H-6107-2015; Giesen, Thomas /B-9476-2015; Schlemmer, Stephan/E-2903-2015; Trappe, Neil/C-9014-2016; Yu, Shanshan/D-8733-2016 OI Martin-Pintado, Jesus/0000-0003-4561-3508; Mueller, Holger/0000-0002-0183-8927; Rimmer, Paul/0000-0002-7180-081X; Giesen, Thomas /0000-0002-2401-0049; Schlemmer, Stephan/0000-0002-1421-7281; Trappe, Neil/0000-0003-2527-9821; FU JPL/Caltech FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri- INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. A part of the work described in this paper was done at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Copyright 2010(C) California Institute of Technology. All rights reserved. NR 38 TC 33 Z9 33 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L47 DI 10.1051/0004-6361/201015117 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900047 ER PT J AU Harwit, M Houde, M Sonnentrucker, P Boogert, ACA Cernicharo, J de Beck, E Decin, L Henkel, C Higgins, RD Jellema, W Kraus, A McCoey, C Melnick, GJ Menten, KM Risacher, C Teyssier, D Vaillancourt, JE Alcolea, J Bujarrabal, V Dominik, C Justtanont, K de Koter, A Marston, AP Olofsson, H Planesas, P Schmidt, M Schoier, FL Szczerba, R Waters, LBFM AF Harwit, M. Houde, M. Sonnentrucker, P. Boogert, A. C. A. Cernicharo, J. de Beck, E. Decin, L. Henkel, C. Higgins, R. D. Jellema, W. Kraus, A. McCoey, C. Melnick, G. J. Menten, K. M. Risacher, C. Teyssier, D. Vaillancourt, J. E. Alcolea, J. Bujarrabal, V. Dominik, C. Justtanont, K. de Koter, A. Marston, A. P. Olofsson, H. Planesas, P. Schmidt, M. Schoier, F. L. Szczerba, R. Waters, L. B. F. M. TI Polarisation observations of VY Canis Majoris H2O 5(32)-4(41) 620.701 GHz maser emission with HIFI SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: AGB and post-AGB; stars: winds, outflows; supergiants; circumstellar matter; masers; reference systems ID LATE-TYPE STARS; EVOLVED STARS; WATER MASERS; LINE; POLARIMETER; MILLIMETER; SHARP AB Context. Water vapour maser emission from evolved oxygen-rich stars remains poorly understood. Additional observations, including polarisation studies and simultaneous observation of different maser transitions may ultimately lead to greater insight. Aims. We have aimed to elucidate the nature and structure of the VY CMa water vapour masers in part by observationally testing a theoretical prediction of the relative strengths of the 620.701 GHz and the 22.235 GHz maser components of ortho H2O. Methods. In its high-resolution mode (HRS) the Herschel Heterodyne Instrument for the Far Infrared (HIFI) offers a frequency resolution of 0.125 MHz, corresponding to a line-of-sight velocity of 0.06 km s(-1), which we employed to obtain the strength and linear polarisation of maser spikes in the spectrum of VY CMa at 620.701 GHz. Simultaneous ground based observations of the 22.235 GHz maser with the Max-Planck-Institut fur Radioastronomie 100-m telescope at Effelsberg, provided a ratio of 620.701 GHz to 22.235 GHz emission. Results. We report the first astronomical detection to date of H2O maser emission at 620.701 GHz. In VY CMa both the 620.701 and the 22.235 GHz polarisation are weak. At 620.701 GHz the maser peaks are superposed on what appears to be a broad emission component, jointly ejected from the star. We observed the 620.701 GHz emission at two epochs 21 days apart, both to measure the potential direction of linearly polarised maser components and to obtain a measure of the longevity of these components. Although we do not detect significant polarisation levels in the core of the line, they rise up to approximately 6% in its wings. C1 [Harwit, M.] Cornell Univ, Ctr Radiophys & Space Res, Washington, DC 20024 USA. [Houde, M.; McCoey, C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Sonnentrucker, P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Boogert, A. C. A.] CALTECH, IPAC, Pasadena, CA 91925 USA. [Cernicharo, J.] CSIC, Madrid 28006, Spain. [de Beck, E.; Decin, L.; Waters, L. B. F. M.] Katholieke Univ Leuven, Inst Sterrenkundeii, B-3001 Heverlee, Belgium. [Henkel, C.; Kraus, A.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Higgins, R. D.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Jellema, W.; Risacher, C.] Univ Groningen, SRON, NL-9700 AV Groningen, Netherlands. [McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Teyssier, D.; Marston, A. P.] European Space Astron Ctr, Madrid 28080, Spain. [Vaillancourt, J. E.] NASA, SOFIA Sci Ctr, Univ Space Res Assoc, Ames Res Ctr, Moffett Field, CA 94035 USA. [Alcolea, J.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Bujarrabal, V.; Planesas, P.] Observ Astron Nacl IGN, Alcala De Henares 28803, Spain. [Decin, L.; Dominik, C.; de Koter, A.; Waters, L. B. F. M.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6525 ED Nijmegen, Netherlands. [Justtanont, K.; Olofsson, H.; Schoier, F. L.] Chalmers, Dept Radio & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [de Koter, A.] Univ Utrecht, Netherlands & Astron Inst, NL-3584 CC Utrecht, Netherlands. [Olofsson, H.] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden. [Planesas, P.] Joint ALMA Observ, Santiago, Chile. [Schmidt, M.; Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. RP Harwit, M (reprint author), Cornell Univ, Ctr Radiophys & Space Res, 511 H St SW, Washington, DC 20024 USA. EM harwit@verizon.net; houde@astro.uwo.ca RI Planesas, Pere/G-7950-2015; OI Planesas, Pere/0000-0002-7808-3040; De Beck, Elvire/0000-0002-7441-7189 FU NASA FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri- INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronmico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. We thank the HIFISTARS consortium for permission to use their VY CMa 556.9 GHz data for calibration purposes. We would like to acknowledge that Tom Phillips first pointed out to us that HIFI might yield useful polarisation observations. And, finally, we extend thanks to the anonymous referee for perceptive insights and suggestions that greatly improved this paper. NR 21 TC 11 Z9 11 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L51 DI 10.1051/0004-6361/201015042 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900051 ER PT J AU Hily-Blant, P Maret, S Bacmann, A Bottinelli, S Parise, B Caux, E Faure, A Bergin, EA Blake, GA Castets, A Ceccarelli, C Cernicharo, J Coutens, A Crimier, N Demyk, K Dominik, C Gerin, M Hennebelle, P Henning, T Kahane, C Klotz, A Melnick, G Pagani, L Schilke, P Vastel, C Wakelam, V Walters, A Baudry, A Bell, T Benedettini, M Boogert, A Cabrit, S Caselli, P Codella, C Comito, C Encrenaz, P Falgarone, E Fuente, A Goldsmith, PF Helmich, F Herbst, E Jacq, T Kama, M Langer, W Lefloch, B Lis, D Lord, S Lorenzani, A Neufeld, D Nisini, B Pacheco, S Phillips, T Salez, M Saraceno, P Schuster, K Tielens, X van der Tak, F van der Wiel, MHD Viti, S Wyrowski, F Yorke, H AF Hily-Blant, P. Maret, S. Bacmann, A. Bottinelli, S. Parise, B. Caux, E. Faure, A. Bergin, E. A. Blake, G. A. Castets, A. Ceccarelli, C. Cernicharo, J. Coutens, A. Crimier, N. Demyk, K. Dominik, C. Gerin, M. Hennebelle, P. Henning, T. Kahane, C. Klotz, A. Melnick, G. Pagani, L. Schilke, P. Vastel, C. Wakelam, V. Walters, A. Baudry, A. Bell, T. Benedettini, M. Boogert, A. Cabrit, S. Caselli, P. Codella, C. Comito, C. Encrenaz, P. Falgarone, E. Fuente, A. Goldsmith, P. F. Helmich, F. Herbst, E. Jacq, T. Kama, M. Langer, W. Lefloch, B. Lis, D. Lord, S. Lorenzani, A. Neufeld, D. Nisini, B. Pacheco, S. Phillips, T. Salez, M. Saraceno, P. Schuster, K. Tielens, X. van der Tak, F. van der Wiel, M. H. D. Viti, S. Wyrowski, F. Yorke, H. TI Nitrogen hydrides in the cold envelope of IRAS 16293-2422 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: abundances; ISM: general; astrochemistry ID DISSOCIATIVE RECOMBINATION; PROTOSTAR IRAS16293-2422; INTERSTELLAR CLOUDS; DARK CLOUDS; CHEMISTRY; NH; MOLECULES; N2H+; SPECTROSCOPY; REGIONS AB Nitrogen is the fifth most abundant element in the Universe, yet the gas-phase chemistry of N-bearing species remains poorly understood. Nitrogen hydrides are key molecules of nitrogen chemistry. Their abundance ratios place strong constraints on the production pathways and reaction rates of nitrogen-bearing molecules. We observed the class 0 protostar IRAS 16293-2422 with the heterodyne instrument HIFI, covering most of the frequency range from 0.48 to 1.78 THz at high spectral resolution. The hyperfine structure of the amidogen radical o-NH2 is resolved and seen in absorption against the continuum of the protostar. Several transitions of ammonia from 1.2 to 1.8 THz are also seen in absorption. These lines trace the low-density envelope of the protostar. Column densities and abundances are estimated for each hydride. We find that NH:NH2:NH3 approximate to 5:1:300. Dark clouds chemical models predict steady-state abundances of NH2 and NH3 in reasonable agreement with the present observations, whilst that of NH is underpredicted by more than one order of magnitude, even using updated kinetic rates. Additional modelling of the nitrogen gas-phase chemistry in dark-cloud conditions is necessary before having recourse to heterogen processes. C1 [Hily-Blant, P.; Maret, S.; Bacmann, A.; Faure, A.; Castets, A.; Ceccarelli, C.; Crimier, N.; Kahane, C.; Lefloch, B.; Pacheco, S.] Univ Grenoble 1, CNRS, Lab Astrophys Grenoble, UMR 5571, Grenoble, France. [Bacmann, A.; Wakelam, V.; Baudry, A.; Jacq, T.] Univ Bordeaux, Lab Astrophys Bordeaux, CNRS, INSU,UMR 5804, Floirac, France. [Boogert, A.; Lord, S.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91109 USA. [Benedettini, M.; Saraceno, P.] Ist Fis Spazio Interplanetario, INAF, Rome, Italy. [Bottinelli, S.; Caux, E.; Coutens, A.; Demyk, K.; Vastel, C.; Walters, A.] Univ Toulouse 3, CNRS, Ctr Etud Spatiale Rayonnements, UMR 5187, F-31062 Toulouse, France. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds, W Yorkshire, England. [Pagani, L.; Cabrit, S.; Encrenaz, P.; Salez, M.] Observ Paris, CNRS, LERMA, F-75014 Paris, France. [Pagani, L.; Cabrit, S.; Encrenaz, P.; Salez, M.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Cernicharo, J.; Crimier, N.] CSIC, INTA, Ctr Astrobiol, Madrid, Spain. [Parise, B.; Schilke, P.; Comito, C.; Wyrowski, F.] Max Planck Inst Radioastron, D-5300 Bonn, Germany. [Codella, C.; Lorenzani, A.] INAF Osservatorio Astrofis Arcetri, Florence, Italy. [Dominik, C.; Kama, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6525 ED Nijmegen, Netherlands. [Fuente, A.] IGN Observ Astron Nacl, Alcala De Henares, Spain. [Goldsmith, P. F.; Langer, W.; Yorke, H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Helmich, F.; van der Tak, F.; van der Wiel, M. H. D.] SRON Netherlands Inst Space Res, Groningen, Netherlands. [Herbst, E.] Ohio State Univ, Columbus, OH 43210 USA. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neufeld, D.] Johns Hopkins Univ, Baltimore, MD USA. [Schilke, P.] Univ Cologne, Inst Phys, Cologne, Germany. [Schuster, K.] Inst Radio Astron Millimetr, Grenoble, France. [Tielens, X.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Viti, S.] UCL, Dept Phys & Astron, London, England. [Nisini, B.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Bergin, E. A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [van der Tak, F.; van der Wiel, M. H. D.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands. [Gerin, M.; Hennebelle, P.; Falgarone, E.] Ecole Normale Super, CNRS, LERMA, UMR 8112, Paris, France. RP Hily-Blant, P (reprint author), Univ Grenoble 1, CNRS, Lab Astrophys Grenoble, UMR 5571, Grenoble, France. RI van der Wiel, Matthijs/M-4531-2014; Coutens, Audrey/M-4533-2014; Fuente, Asuncion/G-1468-2016; Goldsmith, Paul/H-3159-2016; OI van der Wiel, Matthijs/0000-0002-4325-3011; Coutens, Audrey/0000-0003-1805-3920; Fuente, Asuncion/0000-0001-6317-6343; Lorenzani, Andrea/0000-0002-4685-3434; Wakelam, Valentine/0000-0001-9676-2605; Kama, Mihkel/0000-0003-0065-7267; Codella, Claudio/0000-0003-1514-3074; , Brunella Nisini/0000-0002-9190-0113; Maret, Sebastien/0000-0003-1104-4554 NR 38 TC 33 Z9 33 U1 0 U2 9 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L52 DI 10.1051/0004-6361/201015253 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900052 ER PT J AU Johnstone, D Fich, M McCoey, C van Kempen, TA Fuente, A Kristensen, LE Cernicharo, J Caselli, P Visser, R Plume, R Herczeg, GJ van Dishoeck, EF Wampfler, S Bachiller, R Baudry, A Benedettini, M Bergin, E Benz, AO Bjerkeli, P Blake, G Bontemps, S Braine, J Bruderer, S Codella, C Daniel, F di Giorgio, AM Dominik, C Doty, SD Encrenaz, P Giannini, T Goicoechea, JR de Graauw, T Helmich, F Herpin, F Hogerheijde, MR Jacq, T Jorgensen, JK Larsson, B Lis, D Liseau, R Marseille, M Melnick, G Neufeld, D Nisini, B Olberg, M Parise, B Pearson, J Risacher, C Santiago-Garcia, J Saraceno, P Shipman, R Tafalla, M van der Tak, F Wyrowski, F Yildiz, UA Caux, E Honingh, N Jellema, W Schieder, R Teyssier, D Whyborn, N AF Johnstone, D. Fich, M. McCoey, C. van Kempen, T. A. Fuente, A. Kristensen, L. E. Cernicharo, J. Caselli, P. Visser, R. Plume, R. Herczeg, G. J. van Dishoeck, E. F. Wampfler, S. Bachiller, R. Baudry, A. Benedettini, M. Bergin, E. Benz, A. O. Bjerkeli, P. Blake, G. Bontemps, S. Braine, J. Bruderer, S. Codella, C. Daniel, F. di Giorgio, A. M. Dominik, C. Doty, S. D. Encrenaz, P. Giannini, T. Goicoechea, J. R. de Graauw, Th. Helmich, F. Herpin, F. Hogerheijde, M. R. Jacq, T. Jorgensen, J. K. Larsson, B. Lis, D. Liseau, R. Marseille, M. Melnick, G. Neufeld, D. Nisini, B. Olberg, M. Parise, B. Pearson, J. Risacher, C. Santiago-Garcia, J. Saraceno, P. Shipman, R. Tafalla, M. van der Tak, F. Wyrowski, F. Yildiz, U. A. Caux, E. Honingh, N. Jellema, W. Schieder, R. Teyssier, D. Whyborn, N. TI Herschel/HIFI spectroscopy of the intermediate mass protostar NGC7129 FIRS 2 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; stars: formation ID STAR-FORMING REGIONS; YOUNG STELLAR OBJECTS; PACS SPECTROSCOPY; HH 46; WATER; HIFI; EXCITATION; EVOLUTION AB Herschel/HIFI observations of water from the intermediate mass protostar NGC 7129 FIRS 2 provide a powerful diagnostic of the physical conditions in this star formation environment. Six spectral settings, covering four (H2O)-O-16 and two (H2O)-O-18 lines, were observed and all but one (H2O)-O-18 line were detected. The four (H2O)-O-16 lines discussed here share a similar morphology: a narrower, approximate to 6kms(-1), component centered slightly redward of the systemic velocity of NGC7129 FIRS 2 and a much broader, approximate to 25 km s(-1) component centered blueward and likely associated with powerful outflows. The narrower components are consistent with emission from water arising in the envelope around the intermediate mass protostar, and the abundance of H2O is constrained to approximate to 10(-7) for the outer envelope. Additionally, the presence of a narrow self-absorption component for the lowest energy lines is likely due to self-absorption from colder water in the outer envelope. The broader component, where the H2O/CO relative abundance is found to be approximate to 0.2, appears to be tracing the same energetic region that produces strong CO emission at high J. C1 [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G, Canada. [McCoey, C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [van Kempen, T. A.; Kristensen, L. E.; Visser, R.; van Dishoeck, E. F.; Hogerheijde, M. R.; Yildiz, U. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Kempen, T. A.; Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fuente, A.; Bachiller, R.; Santiago-Garcia, J.; Tafalla, M.] Observ Astron Nacl IGN, Alcala De Henares 28800, Spain. [Cernicharo, J.] INTA CSIC, CAB, Dept Astrophys, Torrejon De Ardoz 28850, Spain. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Caselli, P.; Goicoechea, J. R.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Herczeg, G. J.; van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, D-37075 Garching, Germany. [Wampfler, S.; Baudry, A.; Benz, A. O.; Bruderer, S.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Benedettini, M.; Codella, C.; di Giorgio, A. M.; Giannini, T.; Nisini, B.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Benedettini, M.; Bergin, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bjerkeli, P.; Liseau, R.; Olberg, M.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [Blake, G.; Lis, D.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Bontemps, S.; Braine, J.; Herpin, F.; Jacq, T.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Bontemps, S.; Braine, J.; Herpin, F.; Jacq, T.] CNRS INSU, UMR 5804, Floirac, France. [Daniel, F.] Observ Paris, LERMA UMR CNRS 8112, F-92195 Meudon, France. [Daniel, F.] CSIC, Dept Mol & Infrared Astrophys, E-28006 Madrid, Spain. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [Encrenaz, P.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [de Graauw, Th.; Whyborn, N.] Joint ALMA Off, Santiago, Chile. [Helmich, F.; Marseille, M.; Risacher, C.; Shipman, R.; van der Tak, F.; Jellema, W.] SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Parise, B.; Wyrowski, F.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Parise, B.; Honingh, N.; Schieder, R.] Univ Cologne, Inst Phys, KOSMA, D-50937 Cologne, Germany. [Neufeld, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Pearson, J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [van der Tak, F.; Caux, E.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Teyssier, D.] ESA, European Space Astron Ctr, Madrid 28691, Spain. RP Johnstone, D (reprint author), Natl Res Council Canada, Herzberg Inst Astrophys, 5071 W Saanich Rd, Victoria, BC V9E 2E7, Canada. EM doug.johnstone@nrc-cnrc.gc.ca RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Jorgensen, Jes Kristian/L-7936-2014; Wampfler, Susanne/D-2270-2015; Fuente, Asuncion/G-1468-2016; OI , Brunella Nisini/0000-0002-9190-0113; Codella, Claudio/0000-0003-1514-3074; Giannini, Teresa/0000-0002-0224-096X; Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Jorgensen, Jes Kristian/0000-0001-9133-8047; Wampfler, Susanne/0000-0002-3151-7657; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118 FU Spanish MCINN [CSD2009-00038, AYA2006-14786, AYA2009-07304]; National Aeronautics and Space Administration FX We thank the HIFI ICC for all of their help with the data reduction, and both the referee and journal editor for critical comments and speed of response. J.C. and A.F. give thanks to Spanish MCINN for funding support under program CONSOLIDER INGENIO 2010 ref: CSD2009-00038, and J. C., under programs AYA2006-14786 and AYA2009-07304. A portion of this research was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This program is made possible thanks to the HIFI guaranteed time program. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research Groningen, The Netherlands and with major contributions from Germany, France, and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland: NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INT); Sweden: Chalmers University of Technology - MC2, RSS & GARD, Onsala Space Observatory, Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. NR 18 TC 14 Z9 14 U1 1 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L41 DI 10.1051/0004-6361/201015122 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900041 ER PT J AU Justtanont, K Decin, L Schoier, FL Maercker, M Olofsson, H Bujarrabal, V Marston, AP Teyssier, D Alcolea, J Cernicharo, J Dominik, C de Koter, A Melnick, G Menten, K Neufeld, D Planesas, P Schmidt, M Szczerba, R Waters, R de Graauw, T Whyborn, N Finn, T Helmich, F Siebertz, O Schmulling, F Ossenkopf, V Lai, R AF Justtanont, K. Decin, L. Schoier, F. L. Maercker, M. Olofsson, H. Bujarrabal, V. Marston, A. P. Teyssier, D. Alcolea, J. Cernicharo, J. Dominik, C. de Koter, A. Melnick, G. Menten, K. Neufeld, D. Planesas, P. Schmidt, M. Szczerba, R. Waters, R. de Graauw, Th. Whyborn, N. Finn, T. Helmich, F. Siebertz, O. Schmuelling, F. Ossenkopf, V. Lai, R. TI A HIFI preview of warm molecular gas around chi Cygni: first detection of H2O emission toward an S-type AGB star SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: AGB and post-AGB; circumstellar matter; stars: kinematics and dynamics; stars: individual: chi Cyg; stars: late-type; stars: mass-loss ID GIANT BRANCH STARS; MASS-LOSS RATES; CIRCUMSTELLAR WATER-VAPOR; ROTATIONAL LINE-PROFILES; EVOLVED STARS; CARBON STARS; LOSS HISTORY; W-HYDRAE; ISO-SWS; CO AB Aims. A set of new, sensitive, and spectrally resolved, sub-millimeter line observations are used to probe the warm circumstellar gas around the S-type AGB star chi Cyg. The observed lines involve high rotational quantum numbers, which, combined with previously obtained lower-frequency data, make it posible to study in detail the chemical and physical properties of, essentially, the entire circumstellar envelope of chi Cyg. Methods. The data were obtained using the HIFI instrument aboard Herschel, whose high spectral resolution provides valuable information about the line profiles. Detailed, non-LTE, radiative transfer modelling, including dust radiative transfer coupled with a dynamical model, has been performed to derive the temperature, density, and velocity structure of the circumstellar envelope. Results. We report the first detection of circumstellar H2O rotational emission lines in an S-star. Using the high-J CO lines to derive the parameters for the circumstellar envelope, we modelled both the ortho-and para-H2O lines. Our modelling results are consistent with the velocity structure expected for a dust-driven wind. The derived total H2O abundance (relative to H-2) is (1.1 +/- 0.2) x 10(-5), much lower than that in O-rich stars. The derived ortho-to-para ratio of 2.1 +/- 0.6 is close to the high-temperature equilibrium limit, consistent with H2O being formed in the photosphere. C1 [Justtanont, K.; Schoier, F. L.; Olofsson, H.] Chalmers, Onsala Space Observ, Dept Radio & Spece Sci, S-43992 Onsala, Sweden. [Decin, L.; Waters, R.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Decin, L.; Dominik, C.; de Koter, A.; Waters, R.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1098 Amsterdam, Netherlands. [Maercker, M.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Olofsson, H.] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden. [Bujarrabal, V.; Planesas, P.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Marston, A. P.; Teyssier, D.] ESA, European Space Astron Ctr, Madrid 28691, Spain. [Alcolea, J.] Observ Astron Nacl IGN, Madrid 28014, Spain. [de Koter, A.] INTA CSIC, CAB, Madrid 28850, Spain. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6525 ED Nijmegen, Netherlands. [de Koter, A.] Univ Utrecht, Astron Inst, NL-3584 CC Utrecht, Netherlands. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Menten, K.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Neufeld, D.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Planesas, P.] Joint ALMA Observ, Santiago, Chile. [Schmidt, M.; Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. [de Graauw, Th.; Whyborn, N.] Joint ALMA Off, Santiago, Chile. [Finn, T.] Natl Univ Ireland, Expt Phys Dept, Maynooth, Kildare, Ireland. [Helmich, F.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Siebertz, O.; Schmuelling, F.; Ossenkopf, V.] Univ Cologne, Inst Phys 1, KOSMA, D-50937 Cologne, Germany. [Lai, R.] Northrop Grumman Aerosp Syst, Redondo Beach, CA 90278 USA. [Maercker, M.] European So Observ, D-8046 Garching, Germany. RP Justtanont, K (reprint author), Chalmers, Onsala Space Observ, Dept Radio & Spece Sci, S-43992 Onsala, Sweden. EM justtanont@chalmers.se RI Planesas, Pere/G-7950-2015 OI Planesas, Pere/0000-0002-7808-3040 FU Swedish National Space Board; Spanish MICINN [CSD2009-00038]; Polish MNiSW [N 203 393334]; MICINN [AYA2009-07304]; National Aeronautics and Space Administration FX HCSS/HSpot/HIPE is a joint development (are joint developments) by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS and SPIRE consortia. K.J., F.S., M.M., and H.O. acknowledge funding from the Swedish National Space Board. This work has been partially supported by the Spanish MICINN, within the program CONSOLIDER INGENIO 2010, under grant "Molecular Astrophysics: The Herschel and Alma Era - ASTROMOL" (Ref.: CSD2009-00038). R.Sz. and M.Sch. acknowledge support from grant N 203 393334 from Polish MNiSW. J.C. thanks funding from MICINN, grant AYA2009-07304. This research was performed, in part, through a JPL contract funded by the National Aeronautics and Space Administration. NR 45 TC 10 Z9 10 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L6 DI 10.1051/0004-6361/201015092 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900006 ER PT J AU Kama, M Dominik, C Maret, S van der Tak, F Caux, E Ceccarelli, C Fuente, A Crimier, N Lord, S Bacmann, A Baudry, A Bell, T Benedettini, M Bergin, EA Blake, GA Boogert, A Bottinelli, S Cabrit, S Caselli, P Castets, A Cernicharo, J Codella, C Comito, C Coutens, A Demyk, K Encrenaz, P Falgarone, E Gerin, M Goldsmith, PF Helmich, F Hennebelle, P Henning, T Herbst, E Hily-Blant, P Jacq, T Kahane, C Klotz, A Langer, W Lefloch, B Lis, D Lorenzani, A Melnick, G Nisini, B Pacheco, S Pagani, L Parise, B Pearson, J Phillips, T Salez, M Saraceno, P Schilke, P Schuster, K Tielens, X van der Wiel, MHD Vastel, C Viti, S Wakelam, V Walters, A Wyrowski, F Yorke, H Cais, P Gusten, R Philipp, S Klein, T Helmich, F AF Kama, M. Dominik, C. Maret, S. van der Tak, F. Caux, E. Ceccarelli, C. Fuente, A. Crimier, N. Lord, S. Bacmann, A. Baudry, A. Bell, T. Benedettini, M. Bergin, E. A. Blake, G. A. Boogert, A. Bottinelli, S. Cabrit, S. Caselli, P. Castets, A. Cernicharo, J. Codella, C. Comito, C. Coutens, A. Demyk, K. Encrenaz, P. Falgarone, E. Gerin, M. Goldsmith, P. F. Helmich, F. Hennebelle, P. Henning, T. Herbst, E. Hily-Blant, P. Jacq, T. Kahane, C. Klotz, A. Langer, W. Lefloch, B. Lis, D. Lorenzani, A. Melnick, G. Nisini, B. Pacheco, S. Pagani, L. Parise, B. Pearson, J. Phillips, T. Salez, M. Saraceno, P. Schilke, P. Schuster, K. Tielens, X. van der Wiel, M. H. D. Vastel, C. Viti, S. Wakelam, V. Walters, A. Wyrowski, F. Yorke, H. Cais, P. Guesten, R. Philipp, S. Klein, T. Helmich, F. TI The methanol lines and hot core of OMC2-FIR4, an intermediate-mass protostar, with Herschel/HIFI SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; ISM: abundances; ISM: kinematics and dynamics; ISM: molecules ID STAR-FORMING REGIONS; INTERSTELLAR CLOUDS; PACS SPECTROSCOPY; DIAGNOSTIC-TOOL; GAS; EXPLANATION; ENVELOPES; MOLECULES; ABUNDANCE; EMISSION AB In contrast with numerous studies on the physical and chemical structure of low-and high-mass protostars, much less is known about their intermediate-mass counterparts, a class of objects that could help to elucidate the mechanisms of star formation on both ends of the mass range. We present the first results from a rich HIFI spectral dataset on an intermediate-mass protostar, OMC2-FIR4, obtained in the CHESS (Chemical HErschel Survey of Star forming regions) key programme. The more than 100 methanol lines detected between 554 and 961 GHz cover a range in upper level energy of 40 to 540 K. Our physical interpretation focusses on the hot core, but likely the cold envelope and shocked regions also play a role in reality, because an analysis of the line profiles suggests the presence of multiple emission components. An upper limit of 10 (6) is placed on the methanol abundance in the hot core, using a population diagram, large-scale source model and other considerations. This value is consistent with abundances previously seen in low-mass hot cores. Furthermore, the highest energy lines at the highest frequencies display asymmetric profiles, which may arise from infall around the hot core. C1 [Kama, M.; Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6525 ED Nijmegen, Netherlands. [Maret, S.; Ceccarelli, C.; Crimier, N.; Bacmann, A.; Castets, A.; Hily-Blant, P.; Kahane, C.; Lefloch, B.; Pacheco, S.] Univ Grenoble 1, CNRS, UMR 5571, Lab Astrophys Grenoble, Grenoble, France. [van der Tak, F.; Helmich, F.; van der Wiel, M. H. D.; Helmich, F.] SRON Netherlands Inst Space Res, Groningen, Netherlands. [van der Tak, F.; van der Wiel, M. H. D.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands. [Caux, E.; Bottinelli, S.; Coutens, A.; Demyk, K.; Klotz, A.; Vastel, C.; Walters, A.] Univ Toulouse 3, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse, France. [Caux, E.; Bottinelli, S.; Coutens, A.; Demyk, K.; Klotz, A.; Vastel, C.; Walters, A.] CNRS INSU, UMR 5187, Toulouse, France. [Ceccarelli, C.; Bacmann, A.; Baudry, A.; Castets, A.; Jacq, T.; Wakelam, V.; Cais, P.] Univ Bordeaux, Lab Astrophys Bordeaux, Floirac, France. [Ceccarelli, C.; Bacmann, A.; Baudry, A.; Castets, A.; Jacq, T.; Wakelam, V.] CNRS INSU, UMR 5804, Floirac, France. [Fuente, A.] IGN Observ Astron Nacl, Alcala De Henares, Spain. [Crimier, N.; Cernicharo, J.] CSIC INTA, Ctr Astrobiol, Madrid, Spain. [Lord, S.; Boogert, A.] CALTECH, Infared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Benedettini, M.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Rome, Italy. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds, W Yorkshire, England. [Cabrit, S.; Encrenaz, P.; Falgarone, E.; Gerin, M.; Hennebelle, P.; Pagani, L.; Salez, M.] UCP, UPMC, ENS,UMR CNRS INSU 8112, OP,Lab Etud Rayonnement & Matiere Astrophys, Paris, France. [Comito, C.; Parise, B.; Schilke, P.; Wyrowski, F.; Guesten, R.; Philipp, S.; Klein, T.] Max Planck Inst Radioastron, D-5300 Bonn, Germany. [Codella, C.; Lorenzani, A.] INAF Osservatorio Astrofis Arcetri, Florence, Italy. [Goldsmith, P. F.; Langer, W.; Pearson, J.; Yorke, H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Herbst, E.] Ohio State Univ, Columbus, OH 43210 USA. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schilke, P.; Viti, S.] Univ Cologne, Inst Phys, Cologne, Germany. [Schuster, K.] Inst Radio Astron Millimetr, Grenoble, France. [Tielens, X.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Nisini, B.] INAF Osservatorio Astron Roma, Monte Porzio Catone, Italy. [Bergin, E. A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Kama, M (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. RI van der Wiel, Matthijs/M-4531-2014; Coutens, Audrey/M-4533-2014; Fuente, Asuncion/G-1468-2016; Goldsmith, Paul/H-3159-2016; OI van der Wiel, Matthijs/0000-0002-4325-3011; Coutens, Audrey/0000-0003-1805-3920; Fuente, Asuncion/0000-0001-6317-6343; Lorenzani, Andrea/0000-0002-4685-3434; Wakelam, Valentine/0000-0001-9676-2605; Kama, Mihkel/0000-0003-0065-7267; Codella, Claudio/0000-0003-1514-3074; , Brunella Nisini/0000-0002-9190-0113; Maret, Sebastien/0000-0003-1104-4554 FU Netherlands Organisation for Scientific Research (NWO) [021.002.081]; Leids Kerkhoven-Bosscha Fonds FX The authors are grateful to the referee, Dr. Tim van Kempen, for constructive comments leading to a significant improvement of the paper, and to Rens Waters for helpful discussions. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri- INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astron (U) over circle mico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC, and we are deeply grateful to everyone involved in the designing, building, and exploitation of this fantastic instrument. HCSS, HSpot, and HIPE are joint developments by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS, and SPIRE consortia. M. Kama gratefully acknowledges support from the Netherlands Organisation for Scientific Research (NWO) grant number 021.002.081 and the Leids Kerkhoven-Bosscha Fonds, and thanks SRON Groningen for hosting the HIFI ICC volunteers. NR 29 TC 11 Z9 11 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L39 DI 10.1051/0004-6361/201015118 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900039 ER PT J AU Kristensen, LE Visser, R van Dishoeck, EF Yildiz, UA Doty, SD Herczeg, GJ Liu, FC Parise, B Jorgensen, JK van Kempen, TA Brinch, C Wampfler, SF Bruderer, S Benz, AO Hogerheijde, MR Deul, E Bachiller, R Baudry, A Benedettini, M Bergin, EA Bjerkeli, P Blake, GA Bontemps, S Braine, J Caselli, P Cernicharo, J Codella, C Daniel, F de Graauw, T di Giorgio, AM Dominik, C Encrenaz, P Fich, M Fuente, A Giannini, T Goicoechea, JR Helmich, F Herpin, F Jacq, T Johnstone, D Kaufman, MJ Larsson, B Lis, D Liseau, R Marseille, M McCoey, C Melnick, G Neufeld, D Nisini, B Olberg, M Pearson, JC Plume, R Risacher, C Santiago-Garcia, J Saraceno, P Shipman, R Tafalla, M Tielens, AGGM van der Tak, F Wyrowski, F Beintema, D de Jonge, A Dieleman, P Ossenkopf, V Roelfsema, P Stutzki, J Whyborn, N AF Kristensen, L. E. Visser, R. van Dishoeck, E. F. Yildiz, U. A. Doty, S. D. Herczeg, G. J. Liu, F. -C. Parise, B. Jorgensen, J. K. van Kempen, T. A. Brinch, C. Wampfler, S. F. Bruderer, S. Benz, A. O. Hogerheijde, M. R. Deul, E. Bachiller, R. Baudry, A. Benedettini, M. Bergin, E. A. Bjerkeli, P. Blake, G. A. Bontemps, S. Braine, J. Caselli, P. Cernicharo, J. Codella, C. Daniel, F. de Graauw, Th. di Giorgio, A. M. Dominik, C. Encrenaz, P. Fich, M. Fuente, A. Giannini, T. Goicoechea, J. R. Helmich, F. Herpin, F. Jacq, T. Johnstone, D. Kaufman, M. J. Larsson, B. Lis, D. Liseau, R. Marseille, M. McCoey, C. Melnick, G. Neufeld, D. Nisini, B. Olberg, M. Pearson, J. C. Plume, R. Risacher, C. Santiago-Garcia, J. Saraceno, P. Shipman, R. Tafalla, M. Tielens, A. G. G. M. van der Tak, F. Wyrowski, F. Beintema, D. de Jonge, A. Dieleman, P. Ossenkopf, V. Roelfsema, P. Stutzki, J. Whyborn, N. TI Water in low-mass star-forming regions with Herschel HIFI spectroscopy of NGC 1333 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; stars: formation; ISM: molecules; ISM: jets and outflows; ISM: individual objects: NGC 1333 ID PROTOSTELLAR ENVELOPES; PHYSICAL STRUCTURE; NGC-1333 IRAS-4; SUBMILLIMETER; PROTOSTARS; EMISSION; OUTFLOW; ABUNDANCE; VAPOR; DISK AB "Water In Star-forming regions with Herschel" (WISH) is a key programme dedicated to studying the role of water and related species during the star-formation process and constraining the physical and chemical properties of young stellar objects. The Heterodyne Instrument for the Far-Infrared (HIFI) on the Herschel Space Observatory observed three deeply embedded protostars in the low-mass star-forming region NGC 1333 in several (H2O)-O-16, (H2O)-O-18, and CO transitions. Line profiles are resolved for five (H2O)-O-16 transitions in each source, revealing them to be surprisingly complex. The line profiles are decomposed into broad (>20 km s(-1)), medium-broad (similar to 5-10 km s(-1)), and narrow (<5 kms(-1)) components. The (H2O)-O-18 emission is only detected in broad 1(10)-1(01) lines (>20 km s(-1)), indicating that its physical origin is the same as for the broad (H2O)-O-16 component. In one of the sources, IRAS4A, an inverse P Cygni profile is observed, a clear sign of infall in the envelope. From the line profiles alone, it is clear that the bulk of emission arises from shocks, both on small (less than or similar to 1000 AU) and large scales along the outflow cavity walls (similar to 10 000 AU). The H2O line profiles are compared to CO line profiles to constrain the H2O abundance as a function of velocity within these shocked regions. The H2O/CO abundance ratios are measured to be in the range of similar to 0.1-1, corresponding to H2O abundances of similar to 10(-5)-10(-4) with respect to H-2. Approximately 5-10% of the gas is hot enough for all oxygen to be driven into water in warm post-shock gas, mostly at high velocities. C1 [Kristensen, L. E.; Visser, R.; van Dishoeck, E. F.; Yildiz, U. A.; Brinch, C.; Hogerheijde, M. R.; Deul, E.; Tielens, A. G. G. M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.; Herczeg, G. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Liu, F. -C.; Parise, B.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [van Kempen, T. A.; Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wampfler, S. F.; Bruderer, S.; Benz, A. O.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Bachiller, R.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.; Jacq, T.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.; Jacq, T.] CNRS INSU, UMR 5804, Floirac, France. [Benedettini, M.; di Giorgio, A. M.; Saraceno, P.] INAF Inst Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Bergin, E. A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bjerkeli, P.; Liseau, R.; Olberg, M.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Caselli, P.; Codella, C.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] CSIC INTA, Dept Astrofis, Ctr Astrobiol, Madrid 28850, Spain. [de Graauw, Th.; Helmich, F.; Marseille, M.; Risacher, C.; Shipman, R.; van der Tak, F.; Beintema, D.; de Jonge, A.; Dieleman, P.; Roelfsema, P.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [Encrenaz, P.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Fuente, A.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Giannini, T.; Nisini, B.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Kaufman, M. J.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Lis, D.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [McCoey, C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Neufeld, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Santiago-Garcia, J.] Inst Radio Astron Millimetr, E-18012 Granada, Spain. [van der Tak, F.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Ossenkopf, V.; Stutzki, J.] Univ Cologne, Inst Phys 1, KOSMA, D-50937 Cologne, Germany. [Whyborn, N.] Joint ALMA Off, Santiago, Chile. RP Kristensen, LE (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Jorgensen, Jes Kristian/L-7936-2014; Wampfler, Susanne/D-2270-2015; Brinch, Christian/G-5157-2015; Fuente, Asuncion/G-1468-2016; OI Codella, Claudio/0000-0003-1514-3074; Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Jorgensen, Jes Kristian/0000-0001-9133-8047; Wampfler, Susanne/0000-0002-3151-7657; Brinch, Christian/0000-0002-5074-7183; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118; Giannini, Teresa/0000-0002-0224-096X; , Brunella Nisini/0000-0002-9190-0113 NR 22 TC 62 Z9 62 U1 1 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L30 DI 10.1051/0004-6361/201015100 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900030 ER PT J AU Li, HN Christlieb, N Schorck, T Norris, JE Bessell, MS Yong, D Beers, TC Lee, YS Frebel, A Zhao, G AF Li, H. N. Christlieb, N. Schoerck, T. Norris, J. E. Bessell, M. S. Yong, D. Beers, T. C. Lee, Y. S. Frebel, A. Zhao, G. TI The stellar content of the Hamburg/ESO survey VI. Metallicity distribution of main-sequence turnoff stars in the Galactic halo SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Galaxy: halo; surveys; stars: Population II; stars: statistics; stars: abundances ID METAL-POOR STARS; DIGITAL SKY SURVEY; MILKY-WAY TOMOGRAPHY; CHEMICAL EVOLUTION; ABUNDANCE ANALYSIS; HORIZONTAL-BRANCH; Y-2 ISOCHRONES; DATA RELEASE; DWARF STARS; GALAXY AB We determine the metallicity distribution function (MDF) of the Galactic halo based on metal-poor main-sequence turnoff-stars (MSTO) which were selected from the Hamburg/ESO objective-prism survey (HES) database. Corresponding follow-up moderate-resolution observations (R similar to 2000) of 682 stars (among which 617 were accepted program stars) were carried out with the 2.3 m telescope at the Siding Spring Observatory (SSO). Corrections for the survey volume covered by the sample stars were quantitatively estimated and applied to the observed MDF. The corrections are quite small, when compared with those for a previously studied sample of metal-poor giants. The corrected observational MDF of the turnoff sample was then compared with that of the giants, as well as with a number of theoretical predictions of Galactic chemical evolution, including the mass-loss modified simple model. Although the survey-volume corrected MDFs of the metal-poor turnoff and the halo giants notably differ in the region of [Fe/H] > -2.0, below [Fe/H] similar to -2.0, (the region we scientifically focus on most) both MDFs show a sharp drop at [Fe/H] similar to -3.6 and present rather similar distributions in the low-metallicity tail. Theoretical models can fit some parts of the observed MDF, but none is found to simultaneously reproduce the peak as well as the features in the metal-poor region with [Fe/H] between -2.0 to -3.6. Among the tested models only the GAMETE model, when normalized to the tail of the observed MDF below [Fe/H] similar to -3.0, and with Z(cr) = 10(-3.4) Z(circle dot), is able to predict the sharp drop at [Fe/H] similar to -3.6. C1 [Li, H. N.; Zhao, G.] Chinese Acad Sci, Natl Astron Observ, Key Lab Opt Astron, Beijing 100012, Peoples R China. [Li, H. N.; Christlieb, N.; Schoerck, T.] Univ Heidelberg, Zentrum Astron, D-69117 Heidelberg, Germany. [Li, H. N.] Chinese Acad Sci, Grad Univ, Beijing 100080, Peoples R China. [Norris, J. E.; Bessell, M. S.; Yong, D.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Beers, T. C.; Lee, Y. S.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Beers, T. C.; Lee, Y. S.] Michigan State Univ, JINA, E Lansing, MI 48824 USA. [Frebel, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Li, HN (reprint author), Chinese Acad Sci, Natl Astron Observ, Key Lab Opt Astron, A20 Datun Rd, Beijing 100012, Peoples R China. EM lhn@nao.cas.cn; N.Christlieb@lsw.uni-heidelberg.de; jen@mso.anu.edu.au; bessell@mso.anu.edu.au; yong@mso.anu.edu.au; beers@pa.msu.edu; lee@pa.msu.edu; afrebel@cfa.harvard.edu; gzhao@nao.cas.cn FU University of Heidelberg; Deutsche Forschungsgemeinschaft [CH 214/5-1]; Australian Research Council [DP0663562, DP0984924]; US National Science Foundation [PHY 02-16783, PHY 08-22648]; National Natural Science Foundation of China [10821061]; National Basic Research Program of China (973 Program) [2007CB815103]; National Aeronautics and Space Administration; National Science Foundation FX We express our sincere gratitude to the anonymous referee for the constructive comments. H. N. L. would like to thank N. Prantzos, T. Karlsson, and S. Salvadori for providing electronic versions of their theoretical MDF models and helpful comments. H. N. L. and N. C. acknowledge support from the Global Networks program of the University of Heidelberg and from Deutsche Forschungsgemeinschaft under grant CH 214/5-1. Studies at RSAA, ANU, of the most metal-poor stellar populations are supported by Australian Research Council grants DP0663562 and DP0984924, which J.E.N., M. S. B., and D.Y. are pleased to acknowledge. T. C. B. and Y.S.L. acknowledge partial funding of this work from grants PHY 02-16783 and PHY 08-22648: Physics Frontier Center/Joint Institute for Nuclear Astrophysics (JINA), awarded by the US National Science Foundation. This research is partly supported by the National Natural Science Foundation of China under grant No. 10821061 and National Basic Research Program of China (973 Program) under grant No. 2007CB815103, which H. N. L. and G.Z. would like to acknowledge. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 68 TC 22 Z9 22 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR A10 DI 10.1051/0004-6361/201014797 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900071 ER PT J AU Lis, DC Phillips, TG Goldsmith, PF Neufeld, DA Herbst, E Comito, C Schilke, P Muller, HSP Bergin, EA Gerin, M Bell, TA Emprechtinger, M Black, JH Blake, GA Boulanger, F Caux, E Ceccarelli, C Cernicharo, J Coutens, A Crockett, NR Daniel, F Dartois, E De Luca, M Dubernet, ML Encrenaz, P Falgarone, E Geballe, TR Godard, B Giesen, TF Goicoechea, JR Gry, C Gupta, H Hennebelle, P Hily-Blant, P Kolos, R Krelowski, J Joblin, C Johnstone, D Kazmierczak, M Lord, SD Maret, S Martin, PG Martin-Pintado, J Melnick, GJ Menten, KM Monje, R Mookerjea, B Morris, P Murphy, JA Ossenkopf, V Pearson, JC Perault, M Persson, C Plume, R Qin, SL Salez, M Schlemmer, S Schmidt, M Sonnentrucker, P Stutzki, J Teyssier, D Trappe, N van der Tak, FFS Vastel, C Wang, S Yorke, HW Yu, S Zmuidzinas, J Boogert, A Erickson, N Karpov, A Kooi, J Maiwald, FW Schieder, R Zaal, P AF Lis, D. C. Phillips, T. G. Goldsmith, P. F. Neufeld, D. A. Herbst, E. Comito, C. Schilke, P. Mueller, H. S. P. Bergin, E. A. Gerin, M. Bell, T. A. Emprechtinger, M. Black, J. H. Blake, G. A. Boulanger, F. Caux, E. Ceccarelli, C. Cernicharo, J. Coutens, A. Crockett, N. R. Daniel, F. Dartois, E. De Luca, M. Dubernet, M. -L. Encrenaz, P. Falgarone, E. Geballe, T. R. Godard, B. Giesen, T. F. Goicoechea, J. R. Gry, C. Gupta, H. Hennebelle, P. Hily-Blant, P. Kolos, R. Krelowski, J. Joblin, C. Johnstone, D. Kazmierczak, M. Lord, S. D. Maret, S. Martin, P. G. Martin-Pintado, J. Melnick, G. J. Menten, K. M. Monje, R. Mookerjea, B. Morris, P. Murphy, J. A. Ossenkopf, V. Pearson, J. C. Perault, M. Persson, C. Plume, R. Qin, S. -L. Salez, M. Schlemmer, S. Schmidt, M. Sonnentrucker, P. Stutzki, J. Teyssier, D. Trappe, N. van der Tak, F. F. S. Vastel, C. Wang, S. Yorke, H. W. Yu, S. Zmuidzinas, J. Boogert, A. Erickson, N. Karpov, A. Kooi, J. Maiwald, F. W. Schieder, R. Zaal, P. TI Herschel/HIFI measurements of the ortho/para ratio in water towards Sagittarius B2(M) and W31C SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; ISM: abundances; ISM: molecules; molecular processes; submillimeter: ISM ID MOLECULAR CLOUDS; COLOGNE DATABASE; SUBMILLIMETER; SPECTROSCOPY; ABSORPTION; ASTRONOMY; AMMONIA; OXYGEN; VAPOR; CDMS AB We present Herschel/HIFI observations of the fundamental rotational transitions of ortho- and para-(H2O)-O-16 and (H2O)-O-18 in absorption towards Sagittarius B2(M) and W31C. The ortho/para ratio in water in the foreground clouds on the line of sight towards these bright continuum sources is generally consistent with the statistical high-temperature ratio of 3, within the observational uncertainties. However, somewhat unexpectedly, we derive a low ortho/para ratio of 2.35 +/- 0.35, corresponding to a spin temperature of similar to 27 K, towards Sagittarius B2(M) at velocities of the expanding molecular ring. Water molecules in this region appear to have formed with, or relaxed to, an ortho/para ratio close to the value corresponding to the local temperature of the gas and dust. C1 [Lis, D. C.; Phillips, T. G.; Bell, T. A.; Emprechtinger, M.; Blake, G. A.; Monje, R.; Zmuidzinas, J.; Karpov, A.; Kooi, J.] CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA. [Bergin, E. A.; Crockett, N. R.; Wang, S.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Neufeld, D. A.; Sonnentrucker, P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Caux, E.; Coutens, A.; Joblin, C.; Vastel, C.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.; Coutens, A.; Joblin, C.; Vastel, C.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Ceccarelli, C.] Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.; Martin-Pintado, J.] Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Madrid, Spain. [Comito, C.; Schilke, P.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Gerin, M.; Daniel, F.; De Luca, M.; Encrenaz, P.; Falgarone, E.; Godard, B.; Hennebelle, P.; Perault, M.; Salez, M.] Observ Paris, CNRS UMR8112, LERMA, F-75231 Paris 05, France. [Gerin, M.; Daniel, F.; De Luca, M.; Encrenaz, P.; Falgarone, E.; Godard, B.; Hennebelle, P.; Perault, M.; Salez, M.] Ecole Normale Super, F-75231 Paris 05, France. [Dubernet, M. -L.] Univ Paris 06, UMR7092, LPMAA, Paris, France. [Dubernet, M. -L.] Observ Paris, UMR8102, LUTH, Meudon, France. [Schilke, P.; Mueller, H. S. P.; Giesen, T. F.; Ossenkopf, V.; Qin, S. -L.; Schlemmer, S.; Stutzki, J.; Schieder, R.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Goldsmith, P. F.; Gry, C.; Gupta, H.; Pearson, J. C.; Yorke, H. W.; Yu, S.; Maiwald, F. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Lord, S. D.; Morris, P.; Boogert, A.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murphy, J. A.; Trappe, N.] Natl Univ Ireland Maynooth, Maynooth, Kildare, Ireland. [Ossenkopf, V.; van der Tak, F. F. S.; Zaal, P.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Erickson, N.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Black, J. H.; Persson, C.] Chalmers, S-41296 Gothenburg, Sweden. [Boulanger, F.; Dartois, E.] IAS, Orsay, France. [Krelowski, J.; Kazmierczak, M.] Nicholas Copernicus Univ, Torun, Poland. [Geballe, T. R.] Gemini Telescope, Hilo, HI USA. [Kolos, R.] Polish Acad Sci, Inst Phys Chem, Warsaw, Poland. [Mookerjea, B.] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. [Teyssier, D.] ESA, European Space Astron Ctr, Madrid, Spain. RP Lis, DC (reprint author), CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA. EM dcl@caltech.edu RI Goldsmith, Paul/H-3159-2016; Martin-Pintado, Jesus/H-6107-2015; Coutens, Audrey/M-4533-2014; Giesen, Thomas /B-9476-2015; Schlemmer, Stephan/E-2903-2015; Trappe, Neil/C-9014-2016; Yu, Shanshan/D-8733-2016 OI Martin-Pintado, Jesus/0000-0003-4561-3508; Coutens, Audrey/0000-0003-1805-3920; Giesen, Thomas /0000-0002-2401-0049; Mueller, Holger/0000-0002-0183-8927; Maret, Sebastien/0000-0003-1104-4554; Schlemmer, Stephan/0000-0002-1421-7281; Trappe, Neil/0000-0003-2527-9821; FU NASA through JPL/Caltech; NSF [AST-0540882]; National Aeronautics and Space Administration FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology-MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. D. C. L. is supported by the NSF, award AST-0540882 to the CSO. A portion of this research was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 22 TC 40 Z9 40 U1 0 U2 8 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L26 DI 10.1051/0004-6361/201015072 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900026 ER PT J AU Lis, DC Pearson, JC Neufeld, DA Schilke, P Muller, HSP Gupta, H Bell, TA Comito, C Phillips, TG Bergin, EA Ceccarelli, C Goldsmith, PF Blake, GA Bacmann, A Baudry, A Benedettini, M Benz, A Black, J Boogert, A Bottinelli, S Cabrit, S Caselli, P Castets, A Caux, E Cernicharo, J Codella, C Coutens, A Crimier, N Crockett, NR Daniel, F Demyk, K Dominic, C Dubernet, ML Emprechtinger, M Encrenaz, P Falgarone, E Fuente, A Gerin, M Giesen, TF Goicoechea, JR Helmich, F Hennebelle, P Henning, T Herbst, E Hily-Blant, P Hjalmarson, A Hollenbach, D Jack, T Joblin, C Johnstone, D Kahane, C Kama, M Kaufman, M Klotz, A Langer, WD Larsson, B Le Bourlot, J Lefloch, B Le Petit, F Li, D Liseau, R Lord, SD Lorenzani, A Maret, S Martin, PG Melnick, GJ Menten, KM Morris, P Murphy, JA Nagy, Z Nisini, B Ossenkopf, V Pacheco, S Pagani, L Parise, B Perault, M Plume, R Qin, SL Roueff, E Salez, M Sandqvist, A Saraceno, P Schlemmer, S Schuster, K Snell, R Stutzki, J Tielens, A Trappe, N van der Tak, FFS van der Wiel, MHD van Dishoeck, E Vastel, C Viti, S Wakelam, V Walters, A Wang, S Wyrowski, F Yorke, HW Yu, S Zmuidzinas, J Delorme, Y Desbat, JP Gusten, R Krieg, JM Delforge, B AF Lis, D. C. Pearson, J. C. Neufeld, D. A. Schilke, P. Mueller, H. S. P. Gupta, H. Bell, T. A. Comito, C. Phillips, T. G. Bergin, E. A. Ceccarelli, C. Goldsmith, P. F. Blake, G. A. Bacmann, A. Baudry, A. Benedettini, M. Benz, A. Black, J. Boogert, A. Bottinelli, S. Cabrit, S. Caselli, P. Castets, A. Caux, E. Cernicharo, J. Codella, C. Coutens, A. Crimier, N. Crockett, N. R. Daniel, F. Demyk, K. Dominic, C. Dubernet, M. -L. Emprechtinger, M. Encrenaz, P. Falgarone, E. Fuente, A. Gerin, M. Giesen, T. F. Goicoechea, J. R. Helmich, F. Hennebelle, P. Henning, Th. Herbst, E. Hily-Blant, P. Hjalmarson, A. Hollenbach, D. Jack, T. Joblin, C. Johnstone, D. Kahane, C. Kama, M. Kaufman, M. Klotz, A. Langer, W. D. Larsson, B. Le Bourlot, J. Lefloch, B. Le Petit, F. Li, D. Liseau, R. Lord, S. D. Lorenzani, A. Maret, S. Martin, P. G. Melnick, G. J. Menten, K. M. Morris, P. Murphy, J. A. Nagy, Z. Nisini, B. Ossenkopf, V. Pacheco, S. Pagani, L. Parise, B. Perault, M. Plume, R. Qin, S. -L. Roueff, E. Salez, M. Sandqvist, A. Saraceno, P. Schlemmer, S. Schuster, K. Snell, R. Stutzki, J. Tielens, A. Trappe, N. van der Tak, F. F. S. van der Wiel, M. H. D. van Dishoeck, E. Vastel, C. Viti, S. Wakelam, V. Walters, A. Wang, S. Wyrowski, F. Yorke, H. W. Yu, S. Zmuidzinas, J. Delorme, Y. Desbat, J. -P. Guesten, R. Krieg, J. -M. Delforge, B. TI Herschel/HIFI discovery of interstellar chloronium (H2Cl+) SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; line: identification; ISM: abundances; ISM: molecules; molecular processes; submillimetre: ISM ID CHLORINE-BEARING MOLECULES; STAR-FORMING REGION; SPIRAL ARM CLOUDS; NGC 6334 I; HYDROGEN-CHLORIDE; COLOGNE DATABASE; ISOTOPIC RATIO; GROUND-STATE; SUBMILLIMETER; SPECTROSCOPY AB We report the first detection of chloronium, H2Cl+, in the interstellar medium, using the HIFI instrument aboard the Herschel Space Observatory. The 2(12)-1(01) lines of ortho-(H2Cl+)-Cl-35 and ortho-(H2Cl+)-Cl-37 are detected in absorption towards NGC 6334I, and the 1(11)-0(00) transition of para-(H2Cl+)-Cl-35 is detected in absorption towards NGC 6334I and Sgr B2(S). The H2Cl+ column densities are compared to those of the chemically-related species HCl. The derived HCl/H2Cl+ column density ratios, similar to 1-10, are within the range predicted by models of diffuse and dense photon dominated regions (PDRs). However, the observed H2Cl+ column densities, in excess of 10(13) cm(-2), are significantly higher than the model predictions. Our observations demonstrate the outstanding spectroscopic capabilities of HIFI for detecting new interstellar molecules and providing key constraints for astrochemical models. C1 [Lis, D. C.; Bell, T. A.; Phillips, T. G.; Blake, G. A.; Emprechtinger, M.; Zmuidzinas, J.] CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA. [Bergin, E. A.; Crockett, N. R.; Wang, S.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Neufeld, D. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Bottinelli, S.; Caux, E.; Coutens, A.; Demyk, K.; Joblin, C.; Klotz, A.; Vastel, C.; Walters, A.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Bottinelli, S.; Caux, E.; Coutens, A.; Demyk, K.; Joblin, C.; Klotz, A.; Vastel, C.; Walters, A.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Ceccarelli, C.; Bacmann, A.; Castets, A.; Crimier, N.; Hily-Blant, P.; Kahane, C.; Lefloch, B.; Maret, S.; Pacheco, S.] Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France. [Cernicharo, J.; Crimier, N.; Daniel, F.; Goicoechea, J. R.] Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Madrid 28850, Spain. [Schilke, P.; Comito, C.; Menten, K. M.; Parise, B.; Wyrowski, F.; Guesten, R.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Daniel, F.; Falgarone, E.; Gerin, M.; Hennebelle, P.; Perault, M.] Observ Paris, UMR8112, CNRS, LERMA, F-75231 Paris 05, France. [Dubernet, M. -L.] Univ Paris 06, UMR7092, LPMAA, Paris, France. [Dubernet, M. -L.] Observ Paris, UMR8102, LUTH, Meudon, France. [Schilke, P.; Mueller, H. S. P.; Giesen, T. F.; Ossenkopf, V.; Qin, S. -L.; Schlemmer, S.; Stutzki, J.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Pearson, J. C.; Gupta, H.; Goldsmith, P. F.; Langer, W. D.; Li, D.; Morris, P.; Yorke, H. W.; Yu, S.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Daniel, F.; Falgarone, E.; Gerin, M.; Hennebelle, P.; Perault, M.] Ecole Normale Super, F-75231 Paris 05, France. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Boogert, A.; Lord, S. D.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murphy, J. A.; Trappe, N.] Natl Univ Ireland, Maynooth, Kildare, Ireland. [Helmich, F.; Ossenkopf, V.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Nagy, Z.; Plume, R.; van der Tak, F. F. S.; van der Wiel, M. H. D.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Snell, R.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Bacmann, A.; Baudry, A.; Jack, T.; Wakelam, V.; Desbat, J. -P.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Bacmann, A.; Baudry, A.; Jack, T.; Wakelam, V.; Desbat, J. -P.] CNRS INSU, UMR 5804, Floirac, France. [Benedettini, M.; Lorenzani, A.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Rome, Italy. [Cabrit, S.; Encrenaz, P.; Pagani, L.; Salez, M.] Observ Paris, LERMA, UMR 8112, CNRS, Paris, France. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds, W Yorkshire, England. [Codella, C.] INAF Osservatorio Astrofis Arcetri, Florence, Italy. [Dominic, C.; Kama, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. [Dominic, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6525 ED Nijmegen, Netherlands. [Fuente, A.] IGN Observ Astron Nacl, Alcala De Henares, Spain. [Nisini, B.] INAF Osservatorio Astron Roma, Monte Porzio Catone, Italy. [Schuster, K.] Inst RadioAstron Millimetr, Grenoble, France. [Tielens, A.; van Dishoeck, E.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Viti, S.] UCL, Dept Phys & Astron, London, England. [Black, J.; Liseau, R.] Chalmers, Dept Radio & Space Sci, Onsala, Sweden. [Benz, A.] ETH, Inst Astron, CH-8092 Zurich, Switzerland. [Hjalmarson, A.] Chalmers, Onsala Space Observ, Onsala, Sweden. [Hollenbach, D.] SETI Inst, Mountain View, CA USA. [Kaufman, M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Le Bourlot, J.; Le Petit, F.; Roueff, E.] Observ Paris, LUTH, Meudon, France. [Le Bourlot, J.; Le Petit, F.; Roueff, E.] Univ Paris 07, Meudon, France. [Salez, M.; Delorme, Y.; Krieg, J. -M.; Delforge, B.] UCP, UPMC, Inst Lab Etud Rayonnement & Mat Astrophys, UMR 8112,CNRS INSU,OP,ENS, Paris, France. [Henning, Th.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [van der Tak, F. F. S.; van der Wiel, M. H. D.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands. RP Lis, DC (reprint author), CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA. EM dcl@caltech.edu RI Schlemmer, Stephan/E-2903-2015; Trappe, Neil/C-9014-2016; Yu, Shanshan/D-8733-2016; Fuente, Asuncion/G-1468-2016; Goldsmith, Paul/H-3159-2016; van der Wiel, Matthijs/M-4531-2014; Coutens, Audrey/M-4533-2014; Giesen, Thomas /B-9476-2015 OI , Brunella Nisini/0000-0002-9190-0113; Schlemmer, Stephan/0000-0002-1421-7281; Trappe, Neil/0000-0003-2527-9821; Fuente, Asuncion/0000-0001-6317-6343; Lorenzani, Andrea/0000-0002-4685-3434; Mueller, Holger/0000-0002-0183-8927; Codella, Claudio/0000-0003-1514-3074; van der Wiel, Matthijs/0000-0002-4325-3011; Coutens, Audrey/0000-0003-1805-3920; Giesen, Thomas /0000-0002-2401-0049 FU NASA; NSF [AST-0540882] FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri- INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. D. C. L. is supported by the NSF, award AST-0540882 to the CSO. A portion of this research was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 37 TC 48 Z9 48 U1 1 U2 9 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L9 DI 10.1051/0004-6361/201014959 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900009 ER PT J AU Marseille, MG van der Tak, FFS Herpin, F Wyrowski, F Chavarria, L Pietropaoli, B Baudry, A Bontemps, S Cernicharo, J Jacq, T Frieswijk, W Shipman, R van Dishoeck, EF Bachiller, R Benedettini, M Benz, AO Bergin, E Bjerkeli, P Blake, GA Braine, J Bruderer, S Caselli, P Caux, E Codella, C Daniel, F Dieleman, P di Giorgio, AM Dominik, C Doty, SD Encrenaz, P Fich, M Fuente, A Gaier, T Giannini, T Goicoechea, JR de Graauw, T Helmich, F Herczeg, GJ Hogerheijde, MR Jackson, B Javadi, H Jellema, W Johnstone, D Jorgensen, JK Kester, D Kristensen, LE Larsson, B Laauwen, W Lis, D Liseau, R Luinge, W McCoey, C Megej, A Melnick, G Neufeld, D Nisini, B Olberg, M Parise, B Pearson, JC Plume, R Risacher, C Roelfsema, P Santiago-Garcia, J Saraceno, P Siegel, P Stutzki, J Tafalla, M van Kempen, TA Visser, R Wampfler, SF Yildiz, UA AF Marseille, M. G. van der Tak, F. F. S. Herpin, F. Wyrowski, F. Chavarria, L. Pietropaoli, B. Baudry, A. Bontemps, S. Cernicharo, J. Jacq, T. Frieswijk, W. Shipman, R. van Dishoeck, E. F. Bachiller, R. Benedettini, M. Benz, A. O. Bergin, E. Bjerkeli, P. Blake, G. A. Braine, J. Bruderer, S. Caselli, P. Caux, E. Codella, C. Daniel, F. Dieleman, P. di Giorgio, A. M. Dominik, C. Doty, S. D. Encrenaz, P. Fich, M. Fuente, A. Gaier, T. Giannini, T. Goicoechea, J. R. de Graauw, Th. Helmich, F. Herczeg, G. J. Hogerheijde, M. R. Jackson, B. Javadi, H. Jellema, W. Johnstone, D. Jorgensen, J. K. Kester, D. Kristensen, L. E. Larsson, B. Laauwen, W. Lis, D. Liseau, R. Luinge, W. McCoey, C. Megej, A. Melnick, G. Neufeld, D. Nisini, B. Olberg, M. Parise, B. Pearson, J. C. Plume, R. Risacher, C. Roelfsema, P. Santiago-Garcia, J. Saraceno, P. Siegel, P. Stutzki, J. Tafalla, M. van Kempen, T. A. Visser, R. Wampfler, S. F. Yildiz, U. A. TI Water abundances in high-mass protostellar envelopes: Herschel observations with HIFI SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE dust, extinction; ISM: molecules; ISM: abundances ID MONTE-CARLO METHOD; RADIATIVE-TRANSFER; STAR-FORMATION; PROTOSTARS; REGION; EXCITATION; EVOLUTION; EMISSION; CORES; H2O AB Aims. We derive the dense core structure and the water abundance in four massive star-forming regions in the hope of understanding the earliest stages of massive star formation. Methods. We present Herschel/HIFI observations of the para-H2O 1(11)-0(00) and 2(02)-1(11) and the para-(H2O)-O-18 1(11)-0(00) transitions. The envelope contribution to the line profiles is separated from contributions by outflows and foreground clouds. The envelope contribution is modeled with Monte-Carlo radiative transfer codes for dust and molecular lines (MC3D and RATRAN), and the water abundance and the turbulent velocity width as free parameters. Results. While the outflows are mostly seen in emission in high-J lines, envelopes are seen in absorption in ground-state lines, which are almost saturated. The derived water abundances range from 5 x 10(-10) to 4 x 10(-8) in the outer envelopes. We detect cold clouds surrounding the protostar envelope, thanks to the very high quality of the Herschel/HIFI data and the unique ability of water to probe them. Several foreground clouds are also detected along the line of sight. Conclusions. The low H2O abundances in massive dense cores are in accordance with the expectation that high densities and low temperatures lead to freeze-out of water on dust grains. The spread in abundance values is not clearly linked to physical properties of the sources. C1 [Marseille, M. G.; van der Tak, F. F. S.; Frieswijk, W.; Shipman, R.; Dieleman, P.; de Graauw, Th.; Helmich, F.; Jackson, B.; Jellema, W.; Kester, D.; Laauwen, W.; Luinge, W.; Risacher, C.; Roelfsema, P.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [van Dishoeck, E. F.; Hogerheijde, M. R.; Kristensen, L. E.; Visser, R.; Yildiz, U. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.; Herczeg, G. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Benz, A. O.; Bruderer, S.; Wampfler, S. F.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Jacq, T.; Caselli, P.; Codella, C.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Herpin, F.; Chavarria, L.; Pietropaoli, B.; Baudry, A.; Bontemps, S.; Braine, J.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Herpin, F.; Chavarria, L.; Pietropaoli, B.; Baudry, A.; Bontemps, S.; Braine, J.] CNRS INSU, UMR 5804, Floirac, France. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Bjerkeli, P.; Liseau, R.; Olberg, M.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [van der Tak, F. F. S.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Bachiller, R.; Tafalla, M.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Benedettini, M.; di Giorgio, A. M.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Bergin, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] CSIC INTA, Dept Astrofis, Ctr Astrobiol, Madrid 28850, Spain. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [Encrenaz, P.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Fuente, A.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Giannini, T.; Nisini, B.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Lis, D.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [McCoey, C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Melnick, G.; van Kempen, T. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neufeld, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Wyrowski, F.; Parise, B.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Gaier, T.; Javadi, H.; Pearson, J. C.; Siegel, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Santiago-Garcia, J.] Inst Radio Astron Millimetr, Granada 18012, Spain. [Stutzki, J.] Univ Cologne, Inst Phys 1, KOSMA, D-50937 Cologne, Germany. [Megej, A.] ETH, Microwave Lab, CH-8092 Zurich, Switzerland. [Caux, E.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. RP Marseille, MG (reprint author), SRON Netherlands Inst Space Res, POB 800, NL-9700 AV Groningen, Netherlands. EM M.Marseille@sron.nl RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Wampfler, Susanne/D-2270-2015; Fuente, Asuncion/G-1468-2016; OI Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Wampfler, Susanne/0000-0002-3151-7657; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118; Codella, Claudio/0000-0003-1514-3074; Giannini, Teresa/0000-0002-0224-096X; , Brunella Nisini/0000-0002-9190-0113 NR 20 TC 17 Z9 17 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L32 DI 10.1051/0004-6361/201015103 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900032 ER PT J AU Melnick, GJ Tolls, V Neufeld, DA Bergin, EA Phillips, TG Wang, S Crockett, NR Bell, TA Blake, GA Cabrit, S Caux, E Ceccarelli, C Cernicharo, J Comito, C Daniel, F Dubernet, ML Emprechtinger, M Encrenaz, P Falgarone, E Gerin, M Giesen, TF Goicoechea, JR Goldsmith, PF Herbst, E Joblin, C Johnstone, D Langer, WD Latter, WD Lis, DC Lord, SD Maret, S Martin, PG Menten, KM Morris, P Muller, HSP Murphy, JA Ossenkopf, V Pagani, L Pearson, JC Perault, M Plume, R Qin, SL Salez, M Schilke, P Schlemmer, S Stutzki, J Trappe, N van der Tak, FFS Vastel, C Yorke, HW Yu, S Zmuidzinas, J AF Melnick, G. J. Tolls, V. Neufeld, D. A. Bergin, E. A. Phillips, T. G. Wang, S. Crockett, N. R. Bell, T. A. Blake, G. A. Cabrit, S. Caux, E. Ceccarelli, C. Cernicharo, J. Comito, C. Daniel, F. Dubernet, M. -L. Emprechtinger, M. Encrenaz, P. Falgarone, E. Gerin, M. Giesen, T. F. Goicoechea, J. R. Goldsmith, P. F. Herbst, E. Joblin, C. Johnstone, D. Langer, W. D. Latter, W. D. Lis, D. C. Lord, S. D. Maret, S. Martin, P. G. Menten, K. M. Morris, P. Mueller, H. S. P. Murphy, J. A. Ossenkopf, V. Pagani, L. Pearson, J. C. Perault, M. Plume, R. Qin, S. -L. Salez, M. Schilke, P. Schlemmer, S. Stutzki, J. Trappe, N. van der Tak, F. F. S. Vastel, C. Yorke, H. W. Yu, S. Zmuidzinas, J. TI Herschel observations of EXtra-Ordinary Sources (HEXOS): Observations of H2O and its isotopologues towards Orion KL SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: abundances; ISM: molecules ID WAVE-ASTRONOMY-SATELLITE; WATER-VAPOR; SUBMILLIMETER; INSTRUMENT; ABSORPTION; EMISSION; OUTFLOWS; REGION; OMC-1; SWAS AB We report the detection of more than 48 velocity-resolved ground rotational state transitions of (H2O)-O-16, (H2O)-O-18, and (H2O)-O-17 - most for the first time - in both emission and absorption toward Orion KL using Herschel/HIFI. We show that a simple fit, constrained to match the known emission and absorption components along the line of sight, is in excellent agreement with the spectral profiles of all the water lines. Using the measured (H2O)-O-18 line fluxes, which are less affected by line opacity than their (H2O)-O-16 counterparts, and an escape probability method, the column densities of (H2O)-O-18 associated with each emission component are derived. We infer total water abundances of 7.4 x 10(-5), 1.0 x 10(-5), and 1.6 x 10(-5) for the plateau, hot core, and extended warm gas, respectively. In the case of the plateau, this value is consistent with previous measures of the Orion-KL water abundance as well as those of other molecular outflows. In the case of the hot core and extended warm gas, these values are somewhat higher than water abundances derived for other quiescent clouds, suggesting that these regions are likely experiencing enhanced water-ice sublimation from (and reduced freeze-out onto) grain surfaces due to the warmer dust in these sources. C1 [Melnick, G. J.; Tolls, V.] Harvard Smithsonian Ctr Astrophys CfA, Cambridge, MA 02138 USA. [Neufeld, D. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Bergin, E. A.; Wang, S.; Crockett, N. R.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Phillips, T. G.; Bell, T. A.; Emprechtinger, M.; Joblin, C.; Lis, D. C.; Zmuidzinas, J.] CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA. [Blake, G. A.; Joblin, C.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Caux, E.; Vastel, C.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.; Vastel, C.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Ceccarelli, C.; Maret, S.] Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Madrid, Spain. [Comito, C.; Menten, K. M.; Schilke, P.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Daniel, F.; Encrenaz, P.; Falgarone, E.; Gerin, M.; Perault, M.] Observ Paris, CNRS UMR8112, LERMA, F-75231 Paris 05, France. [Daniel, F.; Encrenaz, P.; Falgarone, E.; Gerin, M.; Perault, M.] Ecole Normale Super, F-75231 Paris 05, France. [Dubernet, M. -L.] Univ Paris 06, UMR7092, LPMAA, Paris, France. [Dubernet, M. -L.] Observ Paris, UMR8102, LUTH, Meudon, France. [Giesen, T. F.; Mueller, H. S. P.; Ossenkopf, V.; Qin, S. -L.; Schilke, P.; Schlemmer, S.; Stutzki, J.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Goldsmith, P. F.; Langer, W. D.; Pearson, J. C.; Yorke, H. W.; Yu, S.] Jet Prop Lab, CALTECH, Pasadena, CA 91109 USA. [Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Latter, W. D.; Lord, S. D.; Morris, P.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Murphy, J. A.; Trappe, N.] Natl Univ Ireland Maynooth, Maynooth, Kildare, Ireland. [Ossenkopf, V.; van der Tak, F. F. S.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Cabrit, S.; Pagani, L.; Salez, M.] Observ Paris, LERMA, F-75014 Paris, France. [Cabrit, S.; Pagani, L.; Salez, M.] Observ Paris, CNRS, UMR8112, F-75014 Paris, France. RP Melnick, GJ (reprint author), Harvard Smithsonian Ctr Astrophys CfA, 60 Garden St,Mail Stop 66, Cambridge, MA 02138 USA. EM gmelnick@cfa.harvard.edu RI Goldsmith, Paul/H-3159-2016; Giesen, Thomas /B-9476-2015; Schlemmer, Stephan/E-2903-2015; Trappe, Neil/C-9014-2016; Yu, Shanshan/D-8733-2016 OI Mueller, Holger/0000-0002-0183-8927; Giesen, Thomas /0000-0002-2401-0049; Schlemmer, Stephan/0000-0002-1421-7281; Trappe, Neil/0000-0003-2527-9821; FU NASA through JPL/Caltech; NSF [AST-0540882] FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. CSO is supported by the NSF, award AST-0540882. NR 20 TC 23 Z9 23 U1 1 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L27 DI 10.1051/0004-6361/201015085 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900027 ER PT J AU Menten, KM Wyrowski, F Alcolea, J De Beck, E Decin, L Marston, AP Bujarrabal, V Cernicharo, J Dominik, C Justtanont, K de Koter, A Melnick, G Neufeld, DA Olofsson, H Planesas, P Schmidt, M Schoier, FL Szczerba, R Teyssier, D Waters, LBFM Edwards, K Olberg, M Phillips, TG Morris, P Salez, M Caux, E AF Menten, K. M. Wyrowski, F. Alcolea, J. De Beck, E. Decin, L. Marston, A. P. Bujarrabal, V. Cernicharo, J. Dominik, C. Justtanont, K. de Koter, A. Melnick, G. Neufeld, D. A. Olofsson, H. Planesas, P. Schmidt, M. Schoier, F. L. Szczerba, R. Teyssier, D. Waters, L. B. F. M. Edwards, K. Olberg, M. Phillips, T. G. Morris, P. Salez, M. Caux, E. TI Herschel/HIFI deepens the circumstellar NH3 enigma SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: AGB and post-AGB; supergiants; circumstellar matter ID VY CANIS MAJORIS; INFRARED OBSERVATIONS; INTERSTELLAR AMMONIA; BEARING MOLECULES; INVERSION LINES; MASS-LOSS; IRC+10216; STARS; EMISSION; WATER AB Context. Circumstellar envelopes (CSEs) of a variety of evolved stars have been found to contain ammonia (NH3) in amounts that exceed predictions from conventional chemical models by many orders of magnitude. Aims. The observations reported here were performed in order to better constrain the NH3 abundance in the CSEs of four, quite diverse, oxygen-rich stars using the NH3 ortho J(K) = 1(0)-0(0) ground-state line. Methods. We used the Heterodyne Instrument for the Far Infrared aboard Herschel to observe the NH3 J(K) = 1(0)-0(0) transition near 572.5 GHz, simultaneously with the ortho-H2O J(Ka,Kc) = 1(1,0)-1(0,1) transition, toward VY CMa, OH 26.5+0.6, IRC+10420, and IK Tau. We conducted non-LTE radiative transfer modeling with the goal to derive the NH3 abundance in these objects' CSEs. For the last two stars, Very Large Array imaging of NH3 radio-wavelength inversion lines were used to provide further constraints, particularly on the spatial extent of the NH3-emitting regions. Results. We find remarkably strong NH3 emission in all of our objects with the NH3 line intensities rivaling those of the ground state H2O line. The NH3 abundances relative to H-2 are very high and range from 2 x 10(-7) to 3 x 10(-6) for the objects we have studied. Conclusions. Our observations confirm and even deepen the circumstellar NH3 enigma. While our radiative transfer modeling does not yield satisfactory fits to the observed line profiles, it does lead to abundance estimates that confirm the very high values found in earlier studies. New ways to tackle this mystery will include further Herschel observations of more NH3 lines and imaging with the Expanded Very Large Array. C1 [Menten, K. M.; Wyrowski, F.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Alcolea, J.] Observ Astron Nacl IGN, Madrid 28014, Spain. [De Beck, E.; Decin, L.; Waters, L. B. F. M.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Decin, L.; Waters, L. B. F. M.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1098 Amsterdam, Netherlands. [Marston, A. P.; Dominik, C.; de Koter, A.; Teyssier, D.] ESA, European Space Astron Ctr, Madrid 28691, Spain. [Bujarrabal, V.; Planesas, P.] Observ Astron Nacl IGN, Alcala De Henares 28803, Spain. [Cernicharo, J.] INTA CSIC, CAB, Madrid 28850, Spain. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, Nijmegen, Netherlands. [Justtanont, K.; Olofsson, H.; Schoier, F. L.; Olberg, M.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [de Koter, A.] Univ Utrecht, Astron Inst, NL-3584 CC Utrecht, Netherlands. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neufeld, D. A.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Olofsson, H.] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden. [Schmidt, M.; Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. [Planesas, P.] Joint ALMA Observ, Santiago, Chile. [Edwards, K.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Edwards, K.; Olberg, M.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Phillips, T. G.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Morris, P.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Salez, M.] UCP, UPMC, Lab Etud Rayonnement & Mat Astrophys, UMR 8112,CNRS INSU,OP,ENS, Paris, France. [Salez, M.] Observ Paris, LERMA, F-75014 Paris, France. [Caux, E.] Univ Toulouse UPS, Inst Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. RP Menten, KM (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM kmenten@mpifr.de RI Planesas, Pere/G-7950-2015; OI Planesas, Pere/0000-0002-7808-3040; De Beck, Elvire/0000-0002-7441-7189 FU Spanish MICINN [CSD2009-00038]; Polish MNiSW [N 203 393334]; SNSB; MICINN [AYA2009-07304] FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada, and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France, and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri- INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA); Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. HCSS / HSpot / HIPE is a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS and SPIRE consortia. This work has been partially supported by the Spanish MICINN, within the program CONSOLIDER INGENIO 2010, under grant "Molecular Astrophysics: The Herschel and ALMA Era - ASTROMOL" (ref.: CSD2009-00038). R. Sz. and M. Sch. acknowledge support from grant N 203 393334 from the Polish MNiSW. K. J. acknowledges the funding from SNSB. J. C. thanks funding from MICINN, grant AYA2009-07304. NR 41 TC 25 Z9 25 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L7 DI 10.1051/0004-6361/201015108 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900007 ER PT J AU Neufeld, DA Gonzalez-Alfonso, E Melnick, G Pulecka, M Schmidt, M Szczerba, R Bujarrabal, V Alcolea, J Cernicharo, J Decin, L Dominik, C Justtanont, K de Koter, A Marston, AP Menten, K Olofsson, H Planesas, P Schoier, FL Teyssier, D Waters, LBFM Edwards, K McCoey, C Shipman, R Jellema, W de Graauw, T Ossenkopf, V Schieder, R Philipp, S AF Neufeld, D. A. Gonzalez-Alfonso, E. Melnick, G. Pulecka, M. Schmidt, M. Szczerba, R. Bujarrabal, V. Alcolea, J. Cernicharo, J. Decin, L. Dominik, C. Justtanont, K. de Koter, A. Marston, A. P. Menten, K. Olofsson, H. Planesas, P. Schoier, F. L. Teyssier, D. Waters, L. B. F. M. Edwards, K. McCoey, C. Shipman, R. Jellema, W. de Graauw, T. Ossenkopf, V. Schieder, R. Philipp, S. TI Discovery of water vapour in the carbon star V Cygni from observations with Herschel/HIFI SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: AGB and post-AGB; circumstellar matter; submillimeter: stars ID GIANT BRANCH STARS; CIRCUMSTELLAR ENVELOPES; IRC+10216; EMISSION; SUBMILLIMETER; CHEMISTRY AB We report the discovery of water vapour toward the carbon star V Cygni. We have used Herschel's HIFI instrument, in dual beam switch mode, to observe the 1(11)-0(00) para-water transition at 1113.3430 GHz in the upper sideband of the Band 4b receiver. The observed spectral line profile is nearly parabolic, but with a slight asymmetry associated with blueshifted absorption, and the integrated antenna temperature is 1.69 +/- 0.17 K km s(-1). This detection of thermal water vapour emission, carried out as part of a small survey of water in carbon-rich stars, is only the second such detection toward a carbon-rich AGB star, the first having been obtained by the Submillimeter Wave Astronomy Satellite toward IRC+ 10216. For an assumed ortho-to-para ratio of 3 for water, the observed line intensity implies a water outflow rate similar to 3-6 x 10(-5) Earth masses per year and a water abundance relative to H-2 of similar to 2-5 x 10(-6). This value is a factor of at least 10(4) larger than the expected photospheric abundance in a carbon-rich environment, and - as in IRC+ 10216 - raises the intriguing possibility that the observed water is produced by the vapourisation of orbiting comets or dwarf planets. However, observations of the single line observed to date do not permit us to place strong constraints upon the spatial distribution or origin of the observed water, but future observations of additional transitions will allow us to determine the inner radius of the H2O-emitting zone, and the H2O ortho-to-para ratio, and thereby to place important constraints upon the origin of the observed water emission. C1 [Neufeld, D. A.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Gonzalez-Alfonso, E.] Univ Alcala de Henares, Dept Fis, Madrid 28871, Spain. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pulecka, M.; Schmidt, M.; Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. [Bujarrabal, V.] Observ Astron Nacl IGN, Alcala De Henares 28803, Spain. [Alcolea, J.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Cernicharo, J.] INTA CSIC, CAB, Madrid 28850, Spain. [Decin, L.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Decin, L.; Dominik, C.; de Koter, A.; Waters, L. B. F. M.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1098 Amsterdam, Netherlands. [Justtanont, K.; Olofsson, H.; Schoier, F. L.] Chalmers, Dept Radio & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Marston, A. P.; Teyssier, D.] ESA, European Space Astron Ctr, Madrid 28691, Spain. [Menten, K.; Philipp, S.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Olofsson, H.] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden. [Planesas, P.] Joint ALMA Observ, Santiago, Chile. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, Nijmegen, Netherlands. [de Koter, A.] Univ Utrecht, Astron Inst, NL-3584 CC Utrecht, Netherlands. [Edwards, K.; McCoey, C.] Univ Western Ontario, London, ON N6A 3K7, Canada. [Shipman, R.; Jellema, W.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [de Graauw, T.] Joint ALMA Off, Santiago, Chile. [Ossenkopf, V.; Schieder, R.] Univ Cologne, KOSMA, Inst Phys 1, D-50937 Cologne, Germany. [Edwards, K.; McCoey, C.] Univ Waterloo, Waterloo, ON N2L 3G1, Canada. RP Neufeld, DA (reprint author), Johns Hopkins Univ, 3400 N Charles St, Baltimore, MD 21218 USA. EM neufeld@pha.jhu.edu RI Planesas, Pere/G-7950-2015; OI Planesas, Pere/0000-0002-7808-3040; /0000-0003-1689-9201 FU National Aeronautics and Space Administration; Polish MNiSW [N 203 393334]; Spanish MICINN [CSD2009-00038] FX HIFI has been designed and built by a consortium of institutes and university departments from acrossEurope, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; The Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologa (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. This research was performed, in part, through a JPL contract funded by the National Aeronautics and Space Administration. R.Sz. and M.Sch. acknowledge support from grant N 203 393334 from Polish MNiSW. E.G.-A. is a Research Associate at the Harvard-Smithsonian Center for Astrophysics. This work has been partially supported by the Spanish MICINN, program CONSOLIDER INGENIO 2010, grant ASTROMOL (CSD2009-00038). NR 21 TC 11 Z9 11 U1 1 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L5 DI 10.1051/0004-6361/201015080 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900005 ER PT J AU O'Dwyer, B Del Zanna, G Mason, HE Weber, MA Tripathi, D AF O'Dwyer, B. Del Zanna, G. Mason, H. E. Weber, M. A. Tripathi, D. TI SDO/AIA response to coronal hole, quiet Sun, active region, and flare plasma SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun: activity; Sun: atmosphere; Sun: corona; Sun: UV radiation ID ATOMIC DATABASE; EMISSION-LINES; SOLAR; SPECTROMETER; ANGSTROM; CHIANTI; EIT AB Aims. We examine the contribution of spectral lines and continuum emission to the EUV channels of the Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO) in different regions of the solar atmosphere. Methods. Synthetic spectra were obtained using the CHIANTI atomic database and sample differential emission measures for coronal hole, quiet Sun, active region and flare plasma. These synthetic spectra were convolved with the effective area of each channel, in order to determine the dominant contribution in different regions of the solar atmosphere. Results. We highlight the contribution of particular spectral lines which under certain conditions can affect the interpretation of SDO/AIA data. C1 [O'Dwyer, B.; Del Zanna, G.; Mason, H. E.; Tripathi, D.] Dept Appl Math & Theoret Phys, Cambridge CB3 0WA, England. [Weber, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP O'Dwyer, B (reprint author), Dept Appl Math & Theoret Phys, Wilberforce Rd, Cambridge CB3 0WA, England. EM B.O-Dwyer@damtp.cam.ac.uk; G.Del-Zanna@damtp.cam.ac.uk; H.E.Mason@damtp.cam.ac.uk; mweber@cfa.harvard.edu; D.Tripathi@damtp.cam.ac.uk RI Tripathi, Durgesh/D-9390-2012 OI Tripathi, Durgesh/0000-0003-1689-6254 FU Lockheed-Martin [SP02H1701R]; Gates Cambridge Trust; SAO FX B.O.D., G.D.Z., H.E.M., D.T. acknowledge STFC. M.W. was supported under AIA subcontract SP02H1701R from Lockheed-Martin. B.O.D. was supported by funding from the Gates Cambridge Trust. B.O.D. would like to thank the SAO for providing support for a visit during which this work was initiated. The authors thank Dr. Paul Boerner of the AIA Team for calculating the AIA effective areas. CHIANTI is a collaborative project involving researchers at NRL (USA), and the Universities of: Cambridge (UK), George Mason (USA), and Florence (Italy). NR 18 TC 156 Z9 156 U1 1 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR A21 DI 10.1051/0004-6361/201014872 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900082 ER PT J AU Qin, SL Schilke, P Comito, C Moller, T Rolffs, R Muller, HSP Belloche, A Menten, KM Lis, DC Phillips, TG Bergin, EA Bell, TA Crockett, NR Blake, GA Cabrit, S Caux, E Ceccarelli, C Cernicharo, J Daniel, F Dubernet, ML Emprechtinger, M Encrenaz, P Falgarone, E Gerin, M Giesen, TF Goicoechea, JR Goldsmith, PF Gupta, H Herbst, E Joblin, C Johnstone, D Langer, WD Lord, SD Maret, S Martin, PG Melnick, GJ Morris, P Murphy, JA Neufeld, DA Ossenkopf, V Pagani, L Pearson, JC Perault, M Plume, R Salez, M Schlemmer, S Stutzki, J Trappe, N van der Tak, FFS Vastel, C Wang, S Yorke, HW Yu, S Zmuidzinas, J Boogert, A Gusten, R Hartogh, P Honingh, N Karpov, A Kooi, J Krieg, JM Schieder, R Diez-Gonzalez, MC Bachiller, R Martin-Pintado, J Baechtold, W Olberg, M Nordh, LH Gill, JL Chattopadhyay, G AF Qin, S. -L. Schilke, P. Comito, C. Moeller, T. Rolffs, R. Mueller, H. S. P. Belloche, A. Menten, K. M. Lis, D. C. Phillips, T. G. Bergin, E. A. Bell, T. A. Crockett, N. R. Blake, G. A. Cabrit, S. Caux, E. Ceccarelli, C. Cernicharo, J. Daniel, F. Dubernet, M. -L. Emprechtinger, M. Encrenaz, P. Falgarone, E. Gerin, M. Giesen, T. F. Goicoechea, J. R. Goldsmith, P. F. Gupta, H. Herbst, E. Joblin, C. Johnstone, D. Langer, W. D. Lord, S. D. Maret, S. Martin, P. G. Melnick, G. J. Morris, P. Murphy, J. A. Neufeld, D. A. Ossenkopf, V. Pagani, L. Pearson, J. C. Perault, M. Plume, R. Salez, M. Schlemmer, S. Stutzki, J. Trappe, N. van der Tak, F. F. S. Vastel, C. Wang, S. Yorke, H. W. Yu, S. Zmuidzinas, J. Boogert, A. Guesten, R. Hartogh, P. Honingh, N. Karpov, A. Kooi, J. Krieg, J. -M. Schieder, R. Diez-Gonzalez, M. C. Bachiller, R. Martin-Pintado, J. Baechtold, W. Olberg, M. Nordh, L. H. Gill, J. L. Chattopadhyay, G. TI Herschel observations of EXtra-Ordinary Sources (HEXOS): detecting spiral arm clouds by CH absorption lines SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: abundances; ISM: molecules ID MOLECULAR CLOUDS; SAGITTARIUS B2; COLOGNE DATABASE; SIGHT-LINE; SUBMILLIMETER; SPECTROSCOPY; G10.6-0.4; CHEMISTRY; MICROWAVE; HYDROGEN AB We have observed CH absorption lines (J = 3/2, N = 1 <- J = 1/2, N = 1) against the continuum source Sgr B2(M) using the Herschel/HIFI instrument. With the high spectral resolution and wide velocity coverage provided by HIFI, 31 CH absorption features with different radial velocities and line widths are detected and identified. The narrower line width and lower column density clouds show "spiral arm" cloud characteristics, while the absorption component with the broadest line width and highest column density corresponds to the gas from the Sgr B2 envelope. The observations show that each "spiral arm" harbors multiple velocity components, indicating that the clouds are not uniform and that they have internal structure. This line-of-sight through almost the entire Galaxy offers unique possibilities to study the basic chemistry of simple molecules in diffuse clouds, as a variety of different cloud classes are sampled simultaneously. We find that the linear relationship between CH and H-2 column densities found at lower AV by UV observations does not continue into the range of higher visual extinction. There, the curve flattens, which probably means that CH is depleted in the denser cores of these clouds. C1 [Qin, S. -L.; Schilke, P.; Moeller, T.; Mueller, H. S. P.; Giesen, T. F.; Ossenkopf, V.; Schlemmer, S.; Stutzki, J.; Honingh, N.; Schieder, R.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Schilke, P.; Comito, C.; Rolffs, R.; Belloche, A.; Menten, K. M.; Guesten, R.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Lis, D. C.; Phillips, T. G.; Bell, T. A.; Blake, G. A.; Emprechtinger, M.; Zmuidzinas, J.; Karpov, A.; Kooi, J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Bergin, E. A.; Crockett, N. R.; Wang, S.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Cabrit, S.; Pagani, L.; Salez, M.] LERMA, F-75014 Paris, France. [Cabrit, S.; Pagani, L.; Salez, M.] Observ Paris, CNRS, UMR8112, F-75014 Paris, France. [Caux, E.; Joblin, C.; Vastel, C.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.; Joblin, C.; Vastel, C.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Ceccarelli, C.; Maret, S.] Lab Astrophys Observ Grenoble, F-38041 Grenoble 9, France. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.; Martin-Pintado, J.] Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Madrid 28850, Spain. [Daniel, F.; Encrenaz, P.; Falgarone, E.; Gerin, M.; Perault, M.; Krieg, J. -M.] Observ Paris, UMR8112, CNRS, LERMA, F-75231 Paris 05, France. [Daniel, F.; Encrenaz, P.; Falgarone, E.; Gerin, M.; Perault, M.; Krieg, J. -M.] Ecole Normale Super, F-75231 Paris 05, France. [Dubernet, M. -L.] Univ Paris 06, LPMAA, UMR7092, Paris, France. [Dubernet, M. -L.] Observ Paris, LUTH, UMR8102, Meudon, France. [Goldsmith, P. F.; Gupta, H.; Langer, W. D.; Morris, P.; Pearson, J. C.; Yorke, H. W.; Yu, S.; Gill, J. L.; Chattopadhyay, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Lord, S. D.; Boogert, A.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murphy, J. A.; Trappe, N.] Natl Univ Ireland Maynooth, Maynooth, Kildare, Ireland. [Neufeld, D. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Ossenkopf, V.; van der Tak, F. F. S.] Univ Groningen, SRON Netherlands Inst Space Res, Groningen, Netherlands. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Hartogh, P.] MPI Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Diez-Gonzalez, M. C.; Bachiller, R.] Ctr Astron Yebes, Observ Astron Nacl IGN, E-19080 Guadalajara, Spain. [Baechtold, W.] ETH, Microwave Lab, CH-8092 Zurich, Switzerland. [Olberg, M.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Olberg, M.] Chalmers, S-41296 Gteborg, Sweden. [Nordh, L. H.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. RP Qin, SL (reprint author), Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany. EM qin@ph1.uni-koeln.de RI Trappe, Neil/C-9014-2016; Yu, Shanshan/D-8733-2016; Goldsmith, Paul/H-3159-2016; Martin-Pintado, Jesus/H-6107-2015; Giesen, Thomas /B-9476-2015; Schlemmer, Stephan/E-2903-2015 OI Trappe, Neil/0000-0003-2527-9821; Martin-Pintado, Jesus/0000-0003-4561-3508; Mueller, Holger/0000-0002-0183-8927; Maret, Sebastien/0000-0003-1104-4554; Giesen, Thomas /0000-0002-2401-0049; Schlemmer, Stephan/0000-0002-1421-7281 NR 41 TC 14 Z9 14 U1 0 U2 4 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L14 DI 10.1051/0004-6361/201015107 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900014 ER PT J AU Rolffs, R Schilke, P Comito, C Bergin, EA van der Tak, FFS Lis, DC Qin, SL Menten, KM Gusten, R Bell, TA Blake, GA Caux, E Ceccarelli, C Cernicharo, J Crockett, NR Daniel, F Dubernet, ML Emprechtinger, M Encrenaz, P Gerin, M Giesen, TF Goicoechea, JR Goldsmith, PF Gupta, H Herbst, E Joblin, C Johnstone, D Langer, WD Latter, WD Lord, SD Maret, S Martin, PG Melnick, GJ Morris, P Muller, HSP Murphy, JA Ossenkopf, V Pearson, JC Perault, M Phillips, TG Plume, R Schlemmer, S Stutzki, J Trappe, N Vastel, C Wang, S Yorke, HW Yu, S Zmuidzinas, J Diez-Gonzalez, MC Bachiller, R Martin-Pintado, J Baechtold, W Olberg, M Nordh, LH Gill, JJ Chattopadhyay, G AF Rolffs, R. Schilke, P. Comito, C. Bergin, E. A. van der Tak, F. F. S. Lis, D. C. Qin, S. -L. Menten, K. M. Guesten, R. Bell, T. A. Blake, G. A. Caux, E. Ceccarelli, C. Cernicharo, J. Crockett, N. R. Daniel, F. Dubernet, M. -L. Emprechtinger, M. Encrenaz, P. Gerin, M. Giesen, T. F. Goicoechea, J. R. Goldsmith, P. F. Gupta, H. Herbst, E. Joblin, C. Johnstone, D. Langer, W. D. Latter, W. D. Lord, S. D. Maret, S. Martin, P. G. Melnick, G. J. Morris, P. Mueller, H. S. P. Murphy, J. A. Ossenkopf, V. Pearson, J. C. Perault, M. Phillips, T. G. Plume, R. Schlemmer, S. Stutzki, J. Trappe, N. Vastel, C. Wang, S. Yorke, H. W. Yu, S. Zmuidzinas, J. Diez-Gonzalez, M. C. Bachiller, R. Martin-Pintado, J. Baechtold, W. Olberg, M. Nordh, L. H. Gill, J. J. Chattopadhyay, G. TI Reversal of infall in SgrB2(M) revealed by Herschel/HIFI observations of HCN lines at THz frequencies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; ISM: kinematics and dynamics; ISM: structure; ISM: molecules; ISM: individual objects: SgrB2(M); submillimeter: ISM ID MOLECULAR-SPECTROSCOPY; COLOGNE DATABASE; STAR-FORMATION; FACILITY; OUTFLOW; CDMS; HIFI; B2 AB Aims. To investigate the accretion and feedback processes in massive star formation, we analyze the shapes of emission lines from hot molecular cores, whose asymmetries trace infall and expansion motions. Methods. The high-mass star forming region SgrB2(M) was observed with Herschel/HIFI (HEXOS key project) in various lines of HCN and its isotopologues, complemented by APEX data. The observations are compared to spherically symmetric, centrally heated models with density power-law gradient and different velocity fields (infall or infall+expansion), using the radiative transfer code RATRAN. Results. The HCN line profiles are asymmetric, with the emission peak shifting from blue to red with increasing J and decreasing line opacity (HCN to (HCN)-C-13). This is most evident in the HCN 12-11 line at 1062 GHz. These line shapes are reproduced by a model whose velocity field changes from infall in the outer part to expansion in the inner part. Conclusions. The qualitative reproduction of the HCN lines suggests that infall dominates in the colder, outer regions, but expansion dominates in the warmer, inner regions. We are thus witnessing the onset of feedback in massive star formation, starting to reverse the infall and finally disrupting the whole molecular cloud. To obtain our result, the THz lines uniquely covered by HIFI were critically important. C1 [Rolffs, R.; Schilke, P.; Comito, C.; Menten, K. M.; Guesten, R.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Rolffs, R.; Schilke, P.; Qin, S. -L.; Giesen, T. F.; Mueller, H. S. P.; Ossenkopf, V.; Schlemmer, S.; Stutzki, J.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Bergin, E. A.; Crockett, N. R.; Wang, S.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [van der Tak, F. F. S.; Ossenkopf, V.; Olberg, M.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Lis, D. C.; Bell, T. A.; Emprechtinger, M.; Phillips, T. G.; Zmuidzinas, J.] CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA. [Ceccarelli, C.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Caux, E.; Joblin, C.; Vastel, C.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.; Joblin, C.; Vastel, C.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Ceccarelli, C.; Maret, S.] Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France. [Daniel, F.; Goicoechea, J. R.] Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Madrid 28850, Spain. [Daniel, F.; Encrenaz, P.; Gerin, M.; Perault, M.] Observ Paris, CNRS UMR8112, LERMA, F-75231 Paris 05, France. [Daniel, F.; Encrenaz, P.; Gerin, M.; Perault, M.] Ecole Normale Super, F-75231 Paris 05, France. [Dubernet, M. -L.] Univ Paris 06, UMR7092, LPMAA, Paris, France. [Dubernet, M. -L.] Observ Paris, UMR8102, LUTH, Meudon, France. [Goldsmith, P. F.; Gupta, H.; Langer, W. D.; Pearson, J. C.; Yorke, H. W.; Yu, S.; Gill, J. J.; Chattopadhyay, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Latter, W. D.; Lord, S. D.; Morris, P.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murphy, J. A.; Trappe, N.] Natl Univ Ireland Maynooth, Maynooth, Kildare, Ireland. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Diez-Gonzalez, M. C.; Bachiller, R.] Observ Astron Nacl IGN, Ctr Astron Yebes, Guadalajara 19080, Spain. [Martin-Pintado, J.] CSIC, Inst Estruct Mat, Dept Astrofis Mol & Infrarroja, E-28006 Madrid, Spain. [Baechtold, W.] ETH, Microwave Lab, CH-8092 Zurich, Switzerland. [Olberg, M.] Chalmers, S-41296 Gothenburg, Sweden. [Nordh, L. H.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. RP Rolffs, R (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM rrolffs@mpifr.de RI Goldsmith, Paul/H-3159-2016; Martin-Pintado, Jesus/H-6107-2015; Giesen, Thomas /B-9476-2015; Schlemmer, Stephan/E-2903-2015; Trappe, Neil/C-9014-2016; Yu, Shanshan/D-8733-2016 OI Martin-Pintado, Jesus/0000-0003-4561-3508; Mueller, Holger/0000-0002-0183-8927; Maret, Sebastien/0000-0003-1104-4554; Giesen, Thomas /0000-0002-2401-0049; Schlemmer, Stephan/0000-0002-1421-7281; Trappe, Neil/0000-0003-2527-9821; FU NASA through JPL/Caltech; NSF [AST-0540882] FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri- INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. CSO is supported by the NSF, award AST-0540882. NR 20 TC 16 Z9 16 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L46 DI 10.1051/0004-6361/201015106 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900046 ER PT J AU Salter, DM Kospal, A Getman, KV Hogerheijde, MR van Kempen, TA Carpenter, JM Blake, GA Wilner, D AF Salter, D. M. Kospal, A. Getman, K. V. Hogerheijde, M. R. van Kempen, T. A. Carpenter, J. M. Blake, G. A. Wilner, D. TI Recurring millimeter flares as evidence for star-star magnetic reconnection events in the DQ Tauri PMS binary system SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: individual: DQ Tau; stars: pre-main sequence; binaries: spectroscopic; stars: flare; stars: magnetic field; radio continuum: stars ID CLASSICAL T-TAURI; SPECTROSCOPIC BINARY; SYNCHROTRON RADIATION; UBVRI PHOTOMETRY; SOLAR-FLARES; EMISSION; WAVELENGTHS; FIELDS; BREMSSTRAHLUNG; MODELS AB Observations of the T Tauri spectroscopic binary DQ Tau in April 2008 captured an unusual flare at 3 mm, which peaked at an observed maximum flux of similar to 0.5 Jy (about 27 times the quiescent value). Here we present follow-up millimeter observations that demonstrate a periodicity to the phenomenon. While monitoring 3 new periastron encounters, we have detected flares within 17.5 h (or 4.6%) of the orbital phase of the first reported flare and constrained the main emitting region to a stellar height of 3.7-6.8 R-star. The recorded activity is consistent with the proposed picture for synchrotron emission initiated by a magnetic reconnection event when the two stellar magnetospheres of the highly eccentric (e = 0.556) binary are believed to collide near periastron as the stars approach a minimum separation of 8 R-star (similar to 13 R-circle dot). The similar light curve decay profiles allow us to estimate an average flare duration of 30 h. Assuming one millimeter flare per orbit, DQ Tau could spend approximately 8% of its 15.8-day orbital period in an elevated flux state. These findings continue to serve as a small caution for millimeter flux points in spectral energy distributions that could contain unrecognized flare contributions. Our analysis of the millimeter emission provides an upper limit of 5% on the linear polarization. We discuss the extent to which a severely entangled magnetic field structure and Faraday rotation effects are likely to reduce the observed polarization fraction. We also predict that, for the current picture, the stellar magnetospheres must be misaligned at a significant angle or, alternatively, that the topologies of the outer magnetospheres are poorly described by a well-ordered dipole inside a radius of 7 R-star. Finally, to investigate whether reorganization of the magnetic field during the interaction affects mass accretion, we also present simultaneous optical (VRI) monitoring of the binary, as an established tracer of accretion activity in this system. We find that an accretion event can occur coincident in both time and duration with the synchrotron fallout of a magnetic reconnection event. While the pulsed accretion mechanism has been attributed previously to the dynamical motions of the stars alone, the similarities between the millimeter and optical light curves evoke the possibility of a causal or co-dependent relationship between the magnetospheric and dynamical processes. C1 [Salter, D. M.; Kospal, A.; Hogerheijde, M. R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Getman, K. V.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [van Kempen, T. A.; Wilner, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Carpenter, J. M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Salter, DM (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM demerese@strw.leidenuniv.nl FU Leids Sterrekunde Fonds; Netherlands Organization for Scientific Research FX We would like to thank Vincent Pietu and Jan-Martin Winters at IRAM for their assistance in scheduling and carrying out the observations, as well as Sascha Trippe for help with the PdBI data reduction and analysis. At CARMA we are grateful to Lee Mundy and Nikolaus Volgenau for their assistance in acquiring the data in Director's discretionary time. We would like to thank the observing staff at Teide Observatory for the IAC80 observations, including Alex Oscoz Abad, Cristina Zurita, and Rafael Barrena Delgado. At Wellesley College, we are grateful to Kim McLeod, Wendy Bauer, Steve Slivan and the undergraduate observers Kirsten Levandowski, Kelsey Turbeville, and Kathryn Neugent. Finally, we thank Y. Boehler, A. Dutrey, V. Pietu and S. Guilloteau for communicating data prior to publication. Financial support for travel to Wellesley and IRAM for observational duties was provided by a Leids Sterrekunde Fonds grant. The research of D. M. S., A. K., and M. R. H. is supported through a VIDI grant from the Netherlands Organization for Scientific Research. NR 45 TC 17 Z9 17 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR A32 DI 10.1051/0004-6361/201015197 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900093 ER PT J AU Schilke, P Comito, C Muller, HSP Bergin, EA Herbst, E Lis, DC Neufeld, DA Phillips, TG Bell, TA Blake, GA Cabrit, S Caux, E Ceccarelli, C Cernicharo, J Crockett, NR Daniel, F Dubernet, ML Emprechtinger, M Encrenaz, P Falgarone, E Gerin, M Giesen, TF Goicoechea, JR Goldsmith, PF Gupta, H Joblin, C Johnstone, D Langer, WD Latter, WB Lord, SD Maret, S Martin, PG Melnick, GJ Menten, KM Morris, P Murphy, JA Ossenkopf, V Pagani, L Pearson, JC Perault, M Plume, R Qin, SL Salez, M Schlemmer, S Stutzki, J Trappe, N van der Tak, FFS Vastel, C Wang, S Yorke, HW Yu, S Erickson, N Maiwald, FW Kooi, J Karpov, A Zmuidzinas, J Boogert, A Schieder, R Zaal, P AF Schilke, P. Comito, C. Mueller, H. S. P. Bergin, E. A. Herbst, E. Lis, D. C. Neufeld, D. A. Phillips, T. G. Bell, T. A. Blake, G. A. Cabrit, S. Caux, E. Ceccarelli, C. Cernicharo, J. Crockett, N. R. Daniel, F. Dubernet, M. -L. Emprechtinger, M. Encrenaz, P. Falgarone, E. Gerin, M. Giesen, T. F. Goicoechea, J. R. Goldsmith, P. F. Gupta, H. Joblin, C. Johnstone, D. Langer, W. D. Latter, W. B. Lord, S. D. Maret, S. Martin, P. G. Melnick, G. J. Menten, K. M. Morris, P. Murphy, J. A. Ossenkopf, V. Pagani, L. Pearson, J. C. Perault, M. Plume, R. Qin, S. -L. Salez, M. Schlemmer, S. Stutzki, J. Trappe, N. van der Tak, F. F. S. Vastel, C. Wang, S. Yorke, H. W. Yu, S. Erickson, N. Maiwald, F. W. Kooi, J. Karpov, A. Zmuidzinas, J. Boogert, A. Schieder, R. Zaal, P. TI Herschel observations of ortho- and para-oxidaniumyl (H2O+) in spiral arm clouds toward Sagittarius B2(M) SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; line: profiles; molecular processes ID LASER MAGNETIC-RESONANCE; MOLECULAR-SPECTROSCOPY; COLOGNE DATABASE; SUBMILLIMETER; LINE; BAND; SPECTRUM; B2; HYDROGEN; SPACE AB H2O+ has been observed in its ortho- and para- states toward the massive star forming core Sgr B2(M), located close to the Galactic center. The observations show absorption in all spiral arm clouds between the Sun and Sgr B2. The average o/p ratio of H2O+ in most velocity intervals is 4.8, which corresponds to a nuclear spin temperature of 21 K. The relationship of this spin temperature to the formation temperature and current physical temperature of the gas hosting H2O+ is discussed, but no firm conclusion is reached. In the velocity interval 0-60 km s(-1), an ortho/para ratio of below unity is found, but if this is due to an artifact of contamination by other species or real is not clear. C1 [Schilke, P.; Mueller, H. S. P.; Giesen, T. F.; Schlemmer, S.; Stutzki, J.; Schieder, R.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Schilke, P.; Comito, C.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Bergin, E. A.; Crockett, N. R.; Wang, S.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Lis, D. C.; Phillips, T. G.; Bell, T. A.; Emprechtinger, M.; Kooi, J.; Karpov, A.; Zmuidzinas, J.; Boogert, A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Caux, E.; Joblin, C.; Vastel, C.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.; Joblin, C.; Vastel, C.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Ceccarelli, C.; Maret, S.] Observ Grenoble, Astrophys Lab, F-38041 Grenoble 9, France. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] Lab Astrofis Mol, Ctr Astrobiol CSIC INTA, Madrid, Spain. [Daniel, F.; Encrenaz, P.; Falgarone, E.; Gerin, M.; Perault, M.] Observ Paris, UMR8112, CNRS, LERMA, F-75231 Paris 05, France. [Daniel, F.; Encrenaz, P.; Falgarone, E.; Gerin, M.; Perault, M.] Ecole Normale Super, F-75231 Paris 05, France. [Dubernet, M. -L.] Univ Paris 06, UMR7092, LPMAA, Paris, France. [Dubernet, M. -L.; Ossenkopf, V.] Observ Paris, LUTH, UMR8102, Meudon, France. [Goldsmith, P. F.; Gupta, H.; Langer, W. D.; Pearson, J. C.; Qin, S. -L.; Yorke, H. W.; Yu, S.; Maiwald, F. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Latter, W. B.; Lord, S. D.; Morris, P.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Martin, P. G.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Melnick, G. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murphy, J. A.; Trappe, N.] Natl Univ Ireland Maynooth, Maynooth, Kildare, Ireland. [Neufeld, D. A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Ossenkopf, V.; van der Tak, F. F. S.; Zaal, P.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Erickson, N.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Cabrit, S.; Pagani, L.; Salez, M.] Observ Paris, LERMA, F-75014 Paris, France. [Cabrit, S.; Pagani, L.; Salez, M.; Boogert, A.] Observ Paris, UMR8112, CNRS, F-75014 Paris, France. RP Schilke, P (reprint author), Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany. EM schilke@ph1.uni-koeln.de RI Giesen, Thomas /B-9476-2015; Schlemmer, Stephan/E-2903-2015; Trappe, Neil/C-9014-2016; Yu, Shanshan/D-8733-2016; Goldsmith, Paul/H-3159-2016 OI Giesen, Thomas /0000-0002-2401-0049; Schlemmer, Stephan/0000-0002-1421-7281; Mueller, Holger/0000-0002-0183-8927; Trappe, Neil/0000-0003-2527-9821; FU NASA; NSF [AST-0540882]; Bundesministerium fur Bildung und Forschung (BMBF); Deutsches Zentrum fur Luft- und Raumfahrt (DLR) FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri- INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. CSO is supported by the NSF, award AST-0540882.; H.S.P.M. is very grateful to the Bundesministerium fur Bildung und Forschung (BMBF) for financial support aimed at maintaining the Cologne Database for Molecular Spectroscopy, CDMS. This support has been administered by the Deutsches Zentrum fur Luft- und Raumfahrt (DLR). We appreciate funding for the ASTRONET Project CATS through the Bundesministerium fur Bildung und Forschung (BMBF). NR 37 TC 25 Z9 25 U1 0 U2 7 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L11 DI 10.1051/0004-6361/201015087 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900011 ER PT J AU van der Wiel, MHD van der Tak, FFS Lis, DC Bell, T Bergin, EA Comito, C Emprechtinger, M Schilke, P Caux, E Ceccarelli, C Baudry, A Goldsmith, PF Herbst, E Langer, W Lord, S Neufeld, D Pearson, J Phillips, T Rolffs, R Yorke, H Bacmann, A Benedettini, M Blake, GA Boogert, A Bottinelli, S Cabrit, S Caselli, P Castets, A Cernicharo, J Codella, C Coutens, A Crimier, N Demyk, K Dominik, C Encrenaz, P Falgarone, E Fuente, A Gerin, M Helmich, F Hennebelle, P Henning, T Hily-Blant, P Jacq, T Kahane, C Kama, M Klotz, A Lefloch, B Lorenzani, A Maret, S Melnick, G Nisini, B Pacheco, S Pagani, L Parise, B Salez, M Saraceno, P Schuster, K Tielens, AGGM Vastel, C Viti, S Wakelam, V Walters, A Wyrowski, F Edwards, K Zmuidzinas, J Morris, P Samoska, LA Teyssier, D AF van der Wiel, M. H. D. van der Tak, F. F. S. Lis, D. C. Bell, T. Bergin, E. A. Comito, C. Emprechtinger, M. Schilke, P. Caux, E. Ceccarelli, C. Baudry, A. Goldsmith, P. F. Herbst, E. Langer, W. Lord, S. Neufeld, D. Pearson, J. Phillips, T. Rolffs, R. Yorke, H. Bacmann, A. Benedettini, M. Blake, G. A. Boogert, A. Bottinelli, S. Cabrit, S. Caselli, P. Castets, A. Cernicharo, J. Codella, C. Coutens, A. Crimier, N. Demyk, K. Dominik, C. Encrenaz, P. Falgarone, E. Fuente, A. Gerin, M. Helmich, F. Hennebelle, P. Henning, T. Hily-Blant, P. Jacq, T. Kahane, C. Kama, M. Klotz, A. Lefloch, B. Lorenzani, A. Maret, S. Melnick, G. Nisini, B. Pacheco, S. Pagani, L. Parise, B. Salez, M. Saraceno, P. Schuster, K. Tielens, A. G. G. M. Vastel, C. Viti, S. Wakelam, V. Walters, A. Wyrowski, F. Edwards, K. Zmuidzinas, J. Morris, P. Samoska, L. A. Teyssier, D. TI Herschel/HIFI observations of spectrally resolved methylidyne signatures toward the high-mass star-forming core NGC 6334I SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; ISM: molecules; ISM: individual objects: NGC 6334I ID INTERSTELLAR CLOUDS; MOLECULAR CLOUDS; GROUND-STATE; CH; SPECTROSCOPY; REGIONS; MODELS; ABUNDANCES; NGC-6334; I(N) AB Context. In contrast to the more extensively studied dense star-forming cores, little is known about diffuse gas surrounding star-forming regions. Aims. We study the molecular gas in the Galactic high-mass star-forming region NGC 6334I, which contains diffuse, quiescent components that are inconspicuous in widely used molecular tracers such as CO. Methods. We present Herschel/HIFI observations of methylidyne (CH) toward NGC 6334I observed as part of the "Chemical HErschel Survey of Star forming regions" (CHESS) key program. HIFI resolves each of the six hyperfine components of the lowest rotational transition (J = 3/2-1/2) of CH, observed in both emission and absorption. Results. The CH emission features appear close to the systemic velocity of NGC 6334I, while its measured FWHM linewidth of 3 km s(-1) is smaller than previously observed in dense gas tracers such as NH3 and SiO. The CH abundance in the hot core is similar to 7 x 10(-11), two to three orders of magnitude lower than in diffuse clouds. While other studies find distinct outflows in, e. g., CO and H2O toward NGC 6334I, we do not detect any outflow signatures in CH. At least two redshifted components of cold absorbing material must be present at -3.0 and +6.5 km s(-1) to explain the absorption signatures. We derive a CH column density (N-CH) of 7 x 10(13) and 3 x 10(13) cm(-2) for these two absorbing clouds. We find evidence of two additional absorbing clouds at +8.0 and 0.0 km s(-1), both with N-CH approximate to 2 x 10(13) cm(-2). Turbulent linewidths for the four absorption components vary between 1.5 and 5.0 km s(-1) in FWHM. We constrain the physical properties and locations of the clouds by matching our CH absorbers with the absorption signatures seen in other molecular tracers. Conclusions. In the hot core, molecules such as H2O and CO trace gas that is heated and dynamically influenced by outflow activity, whereas the CH molecule traces more quiescent material. The four CH absorbing clouds have column densities and turbulent properties that are consistent with those of diffuse clouds: two are located in the direct surroundings of NGC 6334, and two are unrelated foreground clouds. Local density and dynamical effects influence the chemical composition of the physical components of NGC 6334, which causes some components to be seen in CH but not in other tracers, and vice versa. C1 [van der Wiel, M. H. D.; van der Tak, F. F. S.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [van der Wiel, M. H. D.; van der Tak, F. F. S.; Helmich, F.] SRON Netherlands Inst Space Res, Groningen, Netherlands. [Goldsmith, P. F.; Langer, W.; Pearson, J.; Yorke, H.; Samoska, L. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bergin, E. A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Comito, C.; Schilke, P.; Rolffs, R.; Parise, B.; Wyrowski, F.] Max Planck Inst Radioastron, D-5300 Bonn, Germany. [Schilke, P.; Rolffs, R.] Univ Cologne, Inst Phys, Cologne, Germany. [Caux, E.; Bottinelli, S.; Coutens, A.; Demyk, K.; Klotz, A.; Vastel, C.; Walters, A.] Univ Toulouse 3, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse, France. [Caux, E.; Bottinelli, S.; Coutens, A.; Demyk, K.; Klotz, A.; Vastel, C.; Walters, A.] CNRS INSU, UMR 5187, Toulouse, France. [Ceccarelli, C.; Bacmann, A.; Castets, A.; Crimier, N.; Hily-Blant, P.; Kahane, C.; Lefloch, B.; Maret, S.; Pacheco, S.] Univ Grenoble 1, CNRS, UMR 5571, Lab Astrophys Grenoble, Grenoble, France. [Ceccarelli, C.; Baudry, A.; Bacmann, A.; Castets, A.; Jacq, T.; Wakelam, V.] Univ Bordeaux, Lab Astrophys Bordeaux, Floirac, France. [Ceccarelli, C.; Baudry, A.; Bacmann, A.; Castets, A.; Jacq, T.; Wakelam, V.] CNRS INSU, UMR 5804, Floirac, France. [Herbst, E.] Ohio State Univ, Columbus, OH 43210 USA. [Benedettini, M.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Rome, Italy. [Lord, S.; Boogert, A.] CALTECH, Infared Proc & Anal Ctr, Pasadena, CA 91109 USA. [Neufeld, D.] Johns Hopkins Univ, Baltimore, MD USA. [Cabrit, S.; Encrenaz, P.; Falgarone, E.; Gerin, M.; Hennebelle, P.; Pagani, L.; Salez, M.] UCP, UPMC, ENS,Lab Etud Rayonnement & Matiere Astrophys, OP,UMR CNRS INSU 8112, Paris, France. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds, W Yorkshire, England. [Cernicharo, J.; Crimier, N.] CSIC INTA, Ctr Astrobiol, Madrid, Spain. [Codella, C.; Lorenzani, A.] INAF Osservatorio Astrofis Arcetri, Florence, Italy. [Dominik, C.; Kama, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6525 ED Nijmegen, Netherlands. [Fuente, A.] IGN Observ Astron Nacl, Alcala De Henares, Spain. [Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nisini, B.] INAF Osservatorio Astron Roma, Monte Porzio Catone, Italy. [Schuster, K.] Inst Radio Astron Millimetr, Grenoble, France. [Viti, S.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Edwards, K.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Teyssier, D.] ESA, European Space Astron Ctr, Madrid, Spain. RP van der Wiel, MHD (reprint author), Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands. EM wiel@astro.rug.nl RI Coutens, Audrey/M-4533-2014; Fuente, Asuncion/G-1468-2016; Goldsmith, Paul/H-3159-2016; van der Wiel, Matthijs/M-4531-2014 OI Coutens, Audrey/0000-0003-1805-3920; Fuente, Asuncion/0000-0001-6317-6343; Lorenzani, Andrea/0000-0002-4685-3434; Wakelam, Valentine/0000-0001-9676-2605; Kama, Mihkel/0000-0003-0065-7267; Codella, Claudio/0000-0003-1514-3074; , Brunella Nisini/0000-0002-9190-0113; Maret, Sebastien/0000-0003-1104-4554; van der Wiel, Matthijs/0000-0002-4325-3011 NR 32 TC 13 Z9 13 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L43 DI 10.1051/0004-6361/201015096 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900043 ER PT J AU Vastel, C Ceccarelli, C Caux, E Coutens, A Cernicharo, J Bottinelli, S Demyk, K Faure, A Wiesenfeld, L Scribano, Y Bacmann, A Hily-Blant, P Maret, S Walters, A Bergin, EA Blake, GA Castets, A Crimier, N Dominik, C Encrenaz, P Gerin, M Hennebelle, P Kahane, C Klotz, A Melnick, G Pagani, L Parise, B Schilke, P Wakelam, V Baudry, A Bell, T Benedettini, M Boogert, A Cabrit, S Caselli, P Codella, C Comito, C Falgarone, E Fuente, A Goldsmith, PF Helmich, F Henning, T Herbst, E Jacq, T Kama, M Langer, W Lefloch, B Lis, D Lord, S Lorenzani, A Neufeld, D Nisini, B Pacheco, S Pearson, J Phillips, T Salez, M Saraceno, P Schuster, K Tielens, X van der Tak, F van der Wiel, MHD Viti, S Wyrowski, F Yorke, H Cais, P Krieg, JM Olberg, M Ravera, L AF Vastel, C. Ceccarelli, C. Caux, E. Coutens, A. Cernicharo, J. Bottinelli, S. Demyk, K. Faure, A. Wiesenfeld, L. Scribano, Y. Bacmann, A. Hily-Blant, P. Maret, S. Walters, A. Bergin, E. A. Blake, G. A. Castets, A. Crimier, N. Dominik, C. Encrenaz, P. Gerin, M. Hennebelle, P. Kahane, C. Klotz, A. Melnick, G. Pagani, L. Parise, B. Schilke, P. Wakelam, V. Baudry, A. Bell, T. Benedettini, M. Boogert, A. Cabrit, S. Caselli, P. Codella, C. Comito, C. Falgarone, E. Fuente, A. Goldsmith, P. F. Helmich, F. Henning, T. Herbst, E. Jacq, T. Kama, M. Langer, W. Lefloch, B. Lis, D. Lord, S. Lorenzani, A. Neufeld, D. Nisini, B. Pacheco, S. Pearson, J. Phillips, T. Salez, M. Saraceno, P. Schuster, K. Tielens, X. van der Tak, F. van der Wiel, M. H. D. Viti, S. Wyrowski, F. Yorke, H. Cais, P. Krieg, J. M. Olberg, M. Ravera, L. TI Ortho-to-para ratio of interstellar heavy water SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; ISM: molecules; submillimeter: ISM; ISM: abundances; molecular processes; line: identification ID PROTOSTAR IRAS 16293-2422; SPECTROSCOPY; CONSTRAINTS; ENVELOPE AB Context. Despite the low elemental deuterium abundance in the Galaxy, enhanced molecular D/H ratios have been found in the environments of low-mass star-forming regions, and in particular the Class 0 protostar IRAS 16293-2422. Aims. The CHESS (Chemical HErschel Surveys of Star forming regions) key program aims to study the molecular complexity of the interstellar medium. The high sensitivity and spectral resolution of the Herschel/HIFI instrument provide a unique opportunity to observe the fundamental 1(1,1)-0(0,0) transition of the ortho-D2O molecule, which is inaccessible from the ground, and determine the ortho-to-para D2O ratio. Methods. We detected the fundamental transition of the ortho-D2O molecule at 607.35 GHz towards IRAS 16293-2422. The line is seen in absorption with a line opacity of 0.62 +/- 0.11 (1 sigma). From the previous ground-based observations of the fundamental 1(1,0)-1(0,1) transition of para-D2O seen in absorption at 316.80 GHz, we estimate a line opacity of 0.26 +/- 0.05 (1 sigma). Results. We show that the observed absorption is caused by the cold gas in the envelope of the protostar. Using these new observations, we estimate for the first time the ortho-to-para D2O ratio to be lower than 2.6 at a 3 sigma level of uncertainty, which should be compared with the thermal equilibrium value of 2:1. C1 [Vastel, C.; Caux, E.; Coutens, A.; Bottinelli, S.; Demyk, K.; Walters, A.; Klotz, A.; Ravera, L.] Univ Toulouse 3, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse, France. [Vastel, C.; Caux, E.; Coutens, A.; Bottinelli, S.; Demyk, K.; Walters, A.; Klotz, A.; Ravera, L.] CNRS INSU, UMR 5187, Toulouse, France. [Ceccarelli, C.; Faure, A.; Wiesenfeld, L.; Bacmann, A.; Hily-Blant, P.; Maret, S.; Castets, A.; Crimier, N.; Kahane, C.; Lefloch, B.; Pacheco, S.] Univ Grenoble 1, CNRS, UMR 5571, Lab Astrophys Grenoble, Grenoble, France. [Ceccarelli, C.; Bacmann, A.; Castets, A.; Wakelam, V.; Baudry, A.; Jacq, T.; Cais, P.] Univ Bordeaux, Lab Astrophys Bordeaux, Floirac, France. [Ceccarelli, C.; Bacmann, A.; Castets, A.; Wakelam, V.; Baudry, A.; Cais, P.] CNRS INSU, UMR 5804, Floirac, France. [Cernicharo, J.; Crimier, N.] CSIC INTA, Ctr Astrobiol, Madrid, Spain. [Scribano, Y.] CNRS, UMR 5209, Lab Interdisciplinaire Carnot Bourgogne, Dijon, France. [Bergin, E. A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Boogert, A.; Lord, S.] CALTECH, Infared Proc & Anal Ctr, Pasadena, CA 91109 USA. [Dominik, C.; Kama, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6525 ED Nijmegen, Netherlands. [Encrenaz, P.; Gerin, M.; Hennebelle, P.; Pagani, L.; Cabrit, S.; Falgarone, E.; Salez, M.; Krieg, J. M.] UCP, UPMC, ENS,UMR CNRS INSU 8112, Lab Etudes Rayonnement & Matiere Astrophys,OP, Paris, France. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Parise, B.; Schilke, P.; Comito, C.; Wyrowski, F.] Max Planck Inst Radioastron, D-5300 Bonn, Germany. [Schilke, P.] Univ Cologne, Inst Phys, Cologne, Germany. [Benedettini, M.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Rome, Italy. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds, W Yorkshire, England. [Codella, C.; Lorenzani, A.] INAF Osservatorio Astrofis Arcetri, Florence, Italy. [Fuente, A.] IGN Observ Astron Nacl, Alcala De Henares, Spain. [Goldsmith, P. F.; Langer, W.; Pearson, J.; Yorke, H.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Helmich, F.; van der Tak, F.; van der Wiel, M. H. D.; Olberg, M.] SRON Netherlands Inst Space Res, Groningen, Netherlands. [Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Neufeld, D.] Ohio State Univ, Columbus, OH 43210 USA. [Nisini, B.] INAF Osservatorio Astron Roma, Monte Porzio Catone, Italy. [Schuster, K.] Inst Radio Astron Millimetr, Grenoble, France. [Tielens, X.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [van der Tak, F.; van der Wiel, M. H. D.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands. [Viti, S.] UCL, Dept Phys & Astron, London, England. [Olberg, M.] Chalmers, Goterborg, Sweden. RP Vastel, C (reprint author), Univ Toulouse 3, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse, France. EM vastel@cesr.fr RI van der Wiel, Matthijs/M-4531-2014; Coutens, Audrey/M-4533-2014; Fuente, Asuncion/G-1468-2016; Goldsmith, Paul/H-3159-2016; OI van der Wiel, Matthijs/0000-0002-4325-3011; Coutens, Audrey/0000-0003-1805-3920; Fuente, Asuncion/0000-0001-6317-6343; Lorenzani, Andrea/0000-0002-4685-3434; Wakelam, Valentine/0000-0001-9676-2605; Kama, Mihkel/0000-0003-0065-7267; Codella, Claudio/0000-0003-1514-3074; , Brunella Nisini/0000-0002-9190-0113; Maret, Sebastien/0000-0003-1104-4554 NR 21 TC 29 Z9 29 U1 1 U2 7 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L31 DI 10.1051/0004-6361/201015101 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900031 ER PT J AU Wampfler, SF Herczeg, GJ Bruderer, S Benz, AO van Dishoeck, EF Kristensen, LE Visser, R Doty, SD Melchior, M van Kempen, TA Yildiz, UA Dedes, C Goicoechea, JR Baudry, A Melnick, G Bachiller, R Benedettini, M Bergin, E Bjerkeli, P Blake, GA Bontemps, S Braine, J Caselli, P Cernicharo, J Codella, C Daniel, F di Giorgio, AM Dominik, C Encrenaz, P Fich, M Fuente, A Giannini, T de Graauw, T Helmich, F Herpin, F Hogerheijde, MR Jacq, T Johnstone, D Jorgensen, JK Larsson, B Lis, D Liseau, R Marseille, M Mc Coey, C Neufeld, D Nisini, B Olberg, M Parise, B Pearson, JC Plume, R Risacher, C Santiago-Garcia, J Saraceno, P Shipman, R Tafalla, M van der Tak, FFS Wyrowski, F Roelfsema, P Jellema, W Dieleman, P Caux, E Stutzki, J AF Wampfler, S. F. Herczeg, G. J. Bruderer, S. Benz, A. O. van Dishoeck, E. F. Kristensen, L. E. Visser, R. Doty, S. D. Melchior, M. van Kempen, T. A. Yildiz, U. A. Dedes, C. Goicoechea, J. R. Baudry, A. Melnick, G. Bachiller, R. Benedettini, M. Bergin, E. Bjerkeli, P. Blake, G. A. Bontemps, S. Braine, J. Caselli, P. Cernicharo, J. Codella, C. Daniel, F. di Giorgio, A. M. Dominik, C. Encrenaz, P. Fich, M. Fuente, A. Giannini, T. de Graauw, Th. Helmich, F. Herpin, F. Hogerheijde, M. R. Jacq, T. Johnstone, D. Jorgensen, J. K. Larsson, B. Lis, D. Liseau, R. Marseille, M. Mc Coey, C. Neufeld, D. Nisini, B. Olberg, M. Parise, B. Pearson, J. C. Plume, R. Risacher, C. Santiago-Garcia, J. Saraceno, P. Shipman, R. Tafalla, M. van der Tak, F. F. S. Wyrowski, F. Roelfsema, P. Jellema, W. Dieleman, P. Caux, E. Stutzki, J. TI Herschel observations of the hydroxyl radical (OH) in young stellar objects SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; stars: formation; ISM: molecules; ISM: jets and outflows; ISM: individual objects: HH 46 ID PHYSICAL STRUCTURE; PACS SPECTROSCOPY; MOLECULAR CLOUD; MASS PROTOSTARS; CLASS-0 SOURCES; CO OBSERVATIONS; FIRS 2; HH 46; EMISSION; PHOTODISSOCIATION AB Aims. "Water In Star-forming regions with Herschel" (WISH) is a Herschel key program investigating the water chemistry in young stellar objects (YSOs) during protostellar evolution. Hydroxyl (OH) is one of the reactants in the chemical network most closely linked to the formation and destruction of H2O. High-temperature (T greater than or similar to 250 K) chemistry connects OH and H2O through the OH + H-2 double left right arrow H2O + H reactions. Formation of H2O from OH is efficient in the high-temperature regime found in shocks and the innermost part of protostellar envelopes. Moreover, in the presence of UV photons, OH can be produced from the photo-dissociation of H2O through H2O + gamma(UV) double right arrow OH + H. Methods. High-resolution spectroscopy of the 163.12 mu m triplet of OH towards HH 46 and NGC 1333 IRAS 2A was carried out with the Heterodyne Instrument for the Far Infrared (HIFI) on board the Herschel Space Observatory. The low-and intermediate-mass protostars HH 46, TMR 1, IRAS 15398-3359, DK Cha, NGC 7129 FIRS 2, and NGC 1333 IRAS 2A were observed with the Photodetector Array Camera and Spectrometer (PACS) on Herschel in four transitions of OH and two [OI] lines. Results. The OH transitions at 79, 84, 119, and 163 mu m and [OI] emission at 63 and 145 mu m were detected with PACS towards the class I low-mass YSOs as well as the intermediate-mass and class I Herbig Ae sources. No OH emission was detected from the class 0 YSO NGC 1333 IRAS 2A, though the 119 mu m was detected in absorption. With HIFI, the 163.12 mu m was not detected from HH 46 and only tentatively detected from NGC 1333 IRAS 2A. The combination of the PACS and HIFI results for HH 46 constrains the line width (FWHM greater than or similar to 11 km s(-1)) and indicates that the OH emission likely originates from shocked gas. This scenario is supported by trends of the OH flux increasing with the [OI] flux and the bolometric luminosity, as found in our sample. Similar OH line ratios for most sources suggest that OH has comparable excitation temperatures despite the different physical properties of the sources. C1 [Wampfler, S. F.; Bruderer, S.; Benz, A. O.; Melchior, M.; Dedes, C.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Herczeg, G. J.; van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [van Dishoeck, E. F.; Kristensen, L. E.; Visser, R.; Yildiz, U. A.; Hogerheijde, M. R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Melchior, M.] Univ Appl Sci NW, Inst Technol 4D, CH-5210 Windisch, Switzerland. [van Kempen, T. A.; Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Goicoechea, J. R.; Cernicharo, J.; Daniel, F.] CSIC INTA, Dept Astrofis, Ctr Astrobiol, Madrid 28850, Spain. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.; Jacq, T.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.; Jacq, T.] CNRS INSU, UMR 5804, Floirac, France. [Bachiller, R.; Tafalla, M.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Benedettini, M.; di Giorgio, A. M.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Bergin, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bjerkeli, P.; Liseau, R.; Olberg, M.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Caselli, P.; Codella, C.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [Encrenaz, P.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Fich, M.; Mc Coey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Fuente, A.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Giannini, T.; Nisini, B.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [de Graauw, Th.; Helmich, F.; Marseille, M.; Risacher, C.; Shipman, R.; van der Tak, F. F. S.; Roelfsema, P.; Jellema, W.; Dieleman, P.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Lis, D.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Mc Coey, C.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Neufeld, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Parise, B.; Wyrowski, F.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Santiago-Garcia, J.] IRAM, E-18012 Granada, Spain. [van der Tak, F. F. S.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Caux, E.] Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France. [Caux, E.] CNRS INSU, UMR 5187, F-31028 Toulouse 4, France. [Stutzki, J.] Univ Cologne, Inst Phys 1, KOSMA, D-50937 Cologne, Germany. RP Wampfler, SF (reprint author), ETH, Inst Astron, CH-8093 Zurich, Switzerland. EM wsusanne@astro.phys.ethz.ch RI Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Jorgensen, Jes Kristian/L-7936-2014; Wampfler, Susanne/D-2270-2015; Fuente, Asuncion/G-1468-2016; Yildiz, Umut/C-5257-2011; OI Kristensen, Lars/0000-0003-1159-3721; Jorgensen, Jes Kristian/0000-0001-9133-8047; Wampfler, Susanne/0000-0002-3151-7657; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118; Codella, Claudio/0000-0003-1514-3074; Yildiz, Umut/0000-0001-6197-2864; Giannini, Teresa/0000-0002-0224-096X; , Brunella Nisini/0000-0002-9190-0113 FU Swiss National Science Foundation [200020-113556] FX The work on star formation at ETH Zurich is partially funded by the Swiss National Science Foundation (grant nr. 200020-113556). This program is made possible thanks to the Swiss HIFI guaranteed time program. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronmico Nacional (IGN), Centro de Astrobiologa (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. NR 35 TC 23 Z9 23 U1 0 U2 9 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L36 DI 10.1051/0004-6361/201015112 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900036 ER PT J AU Wyrowski, F van der Tak, F Herpin, F Baudry, A Bontemps, S Chavarria, L Frieswijk, W Jacq, T Marseille, M Shipman, R van Dishoeck, EF Benz, AO Caselli, P Hogerheijde, MR Johnstone, D Liseau, R Bachiller, R Benedettini, M Bergin, E Bjerkeli, P Blake, G Braine, J Bruderer, S Cernicharo, J Codella, C Daniel, F di Giorgio, AM Dominik, C Doty, SD Encrenaz, P Fich, M Fuente, A Giannini, T Goicoechea, JR de Graauw, T Helmich, F Herczeg, GJ Jorgensen, JK Kristensen, LE Larsson, B Lis, D McCoey, C Melnick, G Nisini, B Olberg, M Parise, B Pearson, JC Plume, R Risacher, C Santiago, J Saraceno, P Tafalla, M van Kempen, TA Visser, R Wampfler, S Yildiz, UA Black, JH Falgarone, E Gerin, M Roelfsema, P Dieleman, P Beintema, D De Jonge, A Whyborn, N Stutzki, J Ossenkopf, V AF Wyrowski, F. van der Tak, F. Herpin, F. Baudry, A. Bontemps, S. Chavarria, L. Frieswijk, W. Jacq, T. Marseille, M. Shipman, R. van Dishoeck, E. F. Benz, A. O. Caselli, P. Hogerheijde, M. R. Johnstone, D. Liseau, R. Bachiller, R. Benedettini, M. Bergin, E. Bjerkeli, P. Blake, G. Braine, J. Bruderer, S. Cernicharo, J. Codella, C. Daniel, F. di Giorgio, A. M. Dominik, C. Doty, S. D. Encrenaz, P. Fich, M. Fuente, A. Giannini, T. Goicoechea, J. R. de Graauw, Th. Helmich, F. Herczeg, G. J. Jorgensen, J. K. Kristensen, L. E. Larsson, B. Lis, D. McCoey, C. Melnick, G. Nisini, B. Olberg, M. Parise, B. Pearson, J. C. Plume, R. Risacher, C. Santiago, J. Saraceno, P. Tafalla, M. van Kempen, T. A. Visser, R. Wampfler, S. Yildiz, U. A. Black, J. H. Falgarone, E. Gerin, M. Roelfsema, P. Dieleman, P. Beintema, D. De Jonge, A. Whyborn, N. Stutzki, J. Ossenkopf, V. TI Variations in H2O+/H2O ratios toward massive star-forming regions SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: clouds; ISM: molecules; submillimeter: ISM; stars: formation ID LASER MAGNETIC-RESONANCE; LINE; ASTRONOMY; CHEMISTRY; SIGHT; DR21; HIFI; W51 AB Early results from the Herschel Space Observatory revealed the water cation H2O+ to be an abundant ingredient of the interstellar medium. Here we present new observations of the H2O and H2O+ lines at 1113.3 and 1115.2 GHz using the Herschel Space Observatory toward a sample of high-mass star-forming regions to observationally study the relation between H2O and H2O+. Nine out of ten sources show absorption from H2O+ in a range of environments: the molecular clumps surrounding the forming and newly formed massive stars, bright high-velocity outflows associated with the massive protostars, and unrelated low-density clouds along the line of sight. Column densities per velocity component of H2O+ are found in the range of 10(12) to a few 10(13) cm(-2). The highest N(H2O+) column densities are found in the outflows of the sources. The ratios of H2O+/H2O are determined in a range from 0.01 to a few and are found to differ strongly between the observed environments with much lower ratios in the massive (proto) cluster envelopes (0.01-0.1) than in outflows and diffuse clouds. Remarkably, even for source components detected in H2O in emission, H2O+ is still seen in absorption. C1 [Wyrowski, F.; Parise, B.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [van der Tak, F.; Marseille, M.; Shipman, R.; Helmich, F.; Dieleman, P.; Beintema, D.; De Jonge, A.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [van der Tak, F.; Frieswijk, W.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Herpin, F.; Baudry, A.; Bontemps, S.; Chavarria, L.; Jacq, T.; Braine, J.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Herpin, F.; Baudry, A.; Bontemps, S.; Chavarria, L.; Jacq, T.; Braine, J.] CNRS INSU, UMR 5804, Floirac, France. [van Dishoeck, E. F.; Herczeg, G. J.] Max Planck Inst Extraterestr Phys, Garching, Germany. [van Dishoeck, E. F.; Hogerheijde, M. R.; Visser, R.; Yildiz, U. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Benz, A. O.; Bruderer, S.; Wampfler, S.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Liseau, R.; Bjerkeli, P.; Olberg, M.; Black, J. H.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [Bachiller, R.; Fuente, A.; Santiago, J.; Tafalla, M.] IGN Observ Astron Nacl, Alcala De Henares 28800, Spain. [Benedettini, M.; Codella, C.; di Giorgio, A. M.; Giannini, T.; Nisini, B.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Benedettini, M.; Bergin, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Blake, G.; Lis, D.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Cernicharo, J.; Goicoechea, J. R.] INTA CSIC, CAB, Dept Astrophys, Torrejon De Ardoz 28850, Spain. [Daniel, F.; Falgarone, E.; Gerin, M.] Observ Paris, LERMA UMR CNRS 8112, F-92195 Meudon, France. [Daniel, F.] CSIC, Dept Mol & Infrared Astrophys, E-28006 Madrid, Spain. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [Encrenaz, P.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [de Graauw, Th.; Whyborn, N.] Joint ALMA Off, Santiago, Chile. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Melnick, G.; van Kempen, T. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Stutzki, J.; Ossenkopf, V.] Univ Cologne, Inst Phys, D-50937 Cologne, Germany. RP Wyrowski, F (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM wyrowski@mpifr-bonn.mpg.de RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; Jorgensen, Jes Kristian/L-7936-2014; Wampfler, Susanne/D-2270-2015; Fuente, Asuncion/G-1468-2016; OI Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Jorgensen, Jes Kristian/0000-0001-9133-8047; Wampfler, Susanne/0000-0002-3151-7657; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118; Codella, Claudio/0000-0003-1514-3074; Giannini, Teresa/0000-0002-0224-096X; , Brunella Nisini/0000-0002-9190-0113 NR 20 TC 22 Z9 22 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L34 DI 10.1051/0004-6361/201015110 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900034 ER PT J AU Yildiz, UA van Dishoeck, EF Kristensen, LE Visser, R Jorgensen, JK Herczeg, GJ van Kempen, TA Hogerheijde, MR Doty, SD Benz, AO Bruderer, S Wampfler, SF Deul, E Bachiller, R Baudry, A Benedettini, M Bergin, E Bjerkeli, P Blake, GA Bontemps, S Braine, J Caselli, P Cernicharo, J Codella, C Daniel, F di Giorgio, AM Dominik, C Encrenaz, P Fich, M Fuente, A Giannini, T Goicoechea, JR de Graauw, T Helmich, F Herpin, F Jacq, T Johnstone, D Larsson, B Lis, D Liseau, R Liu, FC Marseille, M McCoey, C Melnick, G Neufeld, D Nisini, B Olberg, M Parise, B Pearson, JC Plume, R Risacher, C Santiago-Garcia, J Saraceno, P Shipman, R Tafalla, M Tielens, AGGM van der Tak, F Wyrowski, F Dieleman, P Jellema, W Ossenkopf, V Schieder, R Stutzki, J AF Yildiz, U. A. van Dishoeck, E. F. Kristensen, L. E. Visser, R. Jorgensen, J. K. Herczeg, G. J. van Kempen, T. A. Hogerheijde, M. R. Doty, S. D. Benz, A. O. Bruderer, S. Wampfler, S. F. Deul, E. Bachiller, R. Baudry, A. Benedettini, M. Bergin, E. Bjerkeli, P. Blake, G. A. Bontemps, S. Braine, J. Caselli, P. Cernicharo, J. Codella, C. Daniel, F. di Giorgio, A. M. Dominik, C. Encrenaz, P. Fich, M. Fuente, A. Giannini, T. Goicoechea, J. R. de Graauw, Th. Helmich, F. Herpin, F. Jacq, T. Johnstone, D. Larsson, B. Lis, D. Liseau, R. Liu, F. -C. Marseille, M. McCoey, C. Melnick, G. Neufeld, D. Nisini, B. Olberg, M. Parise, B. Pearson, J. C. Plume, R. Risacher, C. Santiago-Garcia, J. Saraceno, P. Shipman, R. Tafalla, M. Tielens, A. G. G. M. van der Tak, F. Wyrowski, F. Dieleman, P. Jellema, W. Ossenkopf, V. Schieder, R. Stutzki, J. TI Herschel/HIFI observations of high-J CO lines in the NGC 1333 low-mass star-forming region SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; stars: formation; ISM: jets and outflows; ISM: molecules ID NGC-1333 IRAS-4; DENSE CORES; PROTOSTARS; ENVELOPES; ABUNDANCE; H2CO; EVOLUTION; WATER; DUST; HIFI AB Herschel/HIFI observations of high-J lines (up to J(u) = 10) of (CO)-C-12, (CO)-C-13 and (CO)-O-18 are presented toward three deeply embedded low-mass protostars, NGC 1333 IRAS 2A, IRAS 4A, and IRAS 4B, obtained as part of the Water In Star-forming regions with Herschel (WISH) key program. The spectrally-resolved HIFI data are complemented by ground-based observations of lower-J CO and isotopologue lines. The (CO)-C-12 10-9 profiles are dominated by broad (FWHM 25-30 km s(-1)) emission. Radiative transfer models are used to constrain the temperature of this shocked gas to 100-200 K. Several CO and (CO)-C-13 line profiles also reveal a medium-broad component (FWHM5-10 km s(-1)), seen prominently in H2O lines. Column densities for both components are presented, providing a reference for determining abundances of other molecules in the same gas. The narrow (CO)-O-18 9-8 lines probe the warmer part of the quiescent envelope. Their intensities require a jump in the CO abundance at an evaporation temperature around 25 K, thus providing new direct evidence for a CO ice evaporation zone around low-mass protostars. C1 [Yildiz, U. A.; van Dishoeck, E. F.; Kristensen, L. E.; Visser, R.; van Kempen, T. A.; Hogerheijde, M. R.; Deul, E.; Tielens, A. G. G. M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.; Herczeg, G. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [van Kempen, T. A.; Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Doty, S. D.] Denison Univ, Dept Phys & Astron, Granville, OH 43023 USA. [Benz, A. O.; Bruderer, S.; Wampfler, S. F.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Bachiller, R.; Tafalla, M.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.; Jacq, T.] Univ Bordeaux, Lab Astrophys Bordeaux, Bordeaux, France. [Baudry, A.; Bontemps, S.; Braine, J.; Herpin, F.; Jacq, T.] CNRS INSU, UMR 5804, Floirac, France. [Benedettini, M.; di Giorgio, A. M.; Saraceno, P.] INAF Ist Fis Spazio Interplanetario, Area Ric Tor Vergata, I-00133 Rome, Italy. [Bergin, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bjerkeli, P.; Liseau, R.; Olberg, M.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Caselli, P.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Caselli, P.; Codella, C.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Cernicharo, J.; Daniel, F.; Goicoechea, J. R.] CSIC INTA, Ctr Astrobiol, Dept Astrofis, Madrid 28850, Spain. [Dominik, C.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Encrenaz, P.] Observ Paris, LERMA, F-75014 Paris, France. [Encrenaz, P.] Observ Paris, CNRS, UMR 8112, F-75014 Paris, France. [Fich, M.; McCoey, C.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Fuente, A.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Giannini, T.; Nisini, B.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [de Graauw, Th.; Helmich, F.; Marseille, M.; Risacher, C.; Shipman, R.; van der Tak, F.; Dieleman, P.; Jellema, W.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Johnstone, D.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Lis, D.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Liu, F. -C.; Parise, B.; Wyrowski, F.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Neufeld, D.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Pearson, J. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Santiago-Garcia, J.] IRAM, E-18012 Granada, Spain. [van der Tak, F.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Ossenkopf, V.; Schieder, R.; Stutzki, J.] Univ Cologne, Inst Phys 1, KOSMA, D-50937 Cologne, Germany. RP Yildiz, UA (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM yildiz@strw.leidenuniv.nl RI Jorgensen, Jes Kristian/L-7936-2014; Wampfler, Susanne/D-2270-2015; Fuente, Asuncion/G-1468-2016; Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Visser, Ruud/J-8574-2012; OI Jorgensen, Jes Kristian/0000-0001-9133-8047; Wampfler, Susanne/0000-0002-3151-7657; Fuente, Asuncion/0000-0001-6317-6343; Bjerkeli, Per/0000-0002-7993-4118; Codella, Claudio/0000-0003-1514-3074; Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Giannini, Teresa/0000-0002-0224-096X; , Brunella Nisini/0000-0002-9190-0113 NR 31 TC 38 Z9 38 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2010 VL 521 AR L40 DI 10.1051/0004-6361/201015119 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 679GW UT WOS:000284150900040 ER PT J AU Dunham, MM Evans, NJ Bourke, TL Myers, PC Huard, TL Stutz, AM AF Dunham, Michael M. Evans, Neal J. Bourke, Tyler L. Myers, Philip C. Huard, Tracy L. Stutz, Amelia M. TI THE SPITZER c2d SURVEY OF NEARBY DENSE CORES. IX. DISCOVERY OF A VERY LOW LUMINOSITY OBJECT DRIVING A MOLECULAR OUTFLOW IN THE DENSE CORE L673-7 SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; ISM: individual objects (L673-7); stars: formation; stars: low-mass ID YOUNG STELLAR OBJECTS; SPECTRAL ENERGY-DISTRIBUTIONS; MULTIBAND IMAGING PHOTOMETER; MASS STAR-FORMATION; T-TAURI STARS; BIPOLAR FLOWS; PROTOSTELLAR ACCRETION; SPACE-TELESCOPE; EMBEDDED SOURCE; LINE FORMATION AB We present new infrared, submillimeter, and millimeter observations of the dense core L673-7 and report the discovery of a low-luminosity, embedded Class 0 protostar driving a molecular outflow. L673-7 is seen in absorption against the mid-infrared background in 5.8, 8, and 24 mu m Spitzer images, allowing for a derivation of the column density profile and total enclosed mass of L673-7, independent of dust temperature assumptions. Estimates of the core mass from these absorption profiles range from 0.2 to 4.5M(circle dot). Millimeter continuum emission indicates a mass of similar to 2M(circle dot), both from a direct calculation assuming isothermal dust and from dust radiative transfer models constrained by the millimeter observations. We use dust radiative transfer models to constrain the internal luminosity of L673-7, defined to be the luminosity of the central source and excluding the luminosity from external heating, to be L-int = 0.01-0.045L(circle dot), with L-int similar to 0.04L(circle dot) the most likely value. L673-7 is thus classified as a very low luminosity object (VeLLO), and is among the lowest luminosity VeLLOs yet studied. We calculate the kinematic and dynamic properties of the molecular outflow in the standard manner. From the outflow properties and standard assumptions regarding the driving of outflows, we calculate the time-averaged protostellar mass accretion rate, total protostellar mass accreted, and expected accretion luminosity to be < M-acc > >= 1.2 x 10(-6) sin i/cos(2) i M-circle dot yr(-1), M-acc >= 0.07 1/cos i M-circle dot, and L-acc >= 0.36L(circle dot), respectively. The discrepancy between this calculated L-acc and the L-int derived from dust radiative transfer models indicates that the current accretion rate is much lower than the average rate over the lifetime of the outflow. Although the protostar embedded within L673-7 is consistent with currently being substellar, it is unlikely to remain as such given the substantial mass reservoir remaining in the core. C1 [Dunham, Michael M.; Evans, Neal J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Bourke, Tyler L.; Myers, Philip C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Huard, Tracy L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Stutz, Amelia M.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Stutz, Amelia M.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Stutz, Amelia M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Dunham, MM (reprint author), Univ Texas Austin, Dept Astron, 1 Univ Stn,C1400, Austin, TX 78712 USA. EM mdunham@astro.as.utexas.edu OI Stutz, Amelia/0000-0003-2300-8200 FU NASA [1224608, 1288664, 1288658, RSA 1377304, NNX 07-AJ72G, 1279198, 1288806]; NSF [AST-0607793]; UT Austin University FX This work is based partly on observations obtained with the Spitzer Space Telescope, operated by the Jet Propulsion Laboratory, California Institute of Technology, and the Caltech Submillimeter Observatory. The authors gratefully acknowledge the assistance of Miranda Dunham in obtaining the CSO 12CO J = 2-1 data, and that of Miwa Block of the MIPS instrument team at Steward Observatory with data reduction. We thank Cornelis Dullemond for reading a draft of this work and providing helpful comments, Jes Jorgensen for his IDL scripts to display three-color images, and the Lorentz Center in Leiden for hosting several meetings that contributed to this paper. This research has made use of NASA's Astrophysics Data System (ADS) Abstract Service and of the SIMBAD database, operated at CDS, Strasbourg, France. Support for this work, part of the Spitzer Legacy Science Program, was provided by NASA through contracts 1224608, 1288664, 1288658, and RSA 1377304. Support was also provided by NASA Origins grant NNX 07-AJ72G and NSF grant AST-0607793. M. M. D. acknowledges partial support from a UT Austin University Continuing Fellowship. Partial support for T. L. B. was provided by NASA through contracts 1279198 and 1288806 issued by the Jet Propulsion Laboratory, California Institute of Technology, to the Smithsonian Astronomical Observatory. NR 108 TC 28 Z9 28 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2010 VL 721 IS 2 BP 995 EP 1013 DI 10.1088/0004-637X/721/2/995 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TP UT WOS:000282193600007 ER PT J AU MacLeod, CL Ivezic, Z Kochanek, CS Kozlowski, S Kelly, B Bullock, E Kimball, A Sesar, B Westman, D Brooks, K Gibson, R Becker, AC de Vries, WH AF MacLeod, C. L. Ivezic, Z. Kochanek, C. S. Kozlowski, S. Kelly, B. Bullock, E. Kimball, A. Sesar, B. Westman, D. Brooks, K. Gibson, R. Becker, A. C. de Vries, W. H. TI MODELING THE TIME VARIABILITY OF SDSS STRIPE 82 QUASARS AS A DAMPED RANDOM WALK SO ASTROPHYSICAL JOURNAL LA English DT Article DE quasars: general ID DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASSES; X-RAY VARIABILITY; OPTICAL VARIABILITY; CONTINUUM VARIABILITY; SPECTRAL VARIABILITY; EDDINGTON RATIO; STELLAR OBJECTS; ACCRETION DISC AB We model the time variability of similar to 9000 spectroscopically confirmed quasars in SDSS Stripe 82 as a damped random walk (DRW). Using 2.7 million photometric measurements collected over 10 yr, we confirm the results of Kelly et al. and Kozlowski et al. that this model can explain quasar light curves at an impressive fidelity level (0.01-0.02 mag). The DRW model provides a simple, fast (O(N) for N data points), and powerful statistical description of quasar light curves by a characteristic timescale (tau) and an asymptotic rms variability on long timescales (SF infinity). We searched for correlations between these two variability parameters and physical parameters such as luminosity and black hole mass, and rest-frame wavelength. Our analysis shows SF infinity to increase with decreasing luminosity and rest-frame wavelength as observed previously, and without a correlation with redshift. We find a correlation between SF infinity and black hole mass with a power-law index of 0.18 +/- 0.03, independent of the anti-correlation with luminosity. We find that t increases with increasing wavelength with a power-law index of 0.17, remains nearly constant with redshift and luminosity, and increases with increasing black hole mass with a power-law index of 0.21 +/- 0.07. The amplitude of variability is anti-correlated with the Eddington ratio, which suggests a scenario where optical fluctuations are tied to variations in the accretion rate. However, we find an additional dependence on luminosity and/or black hole mass that cannot be explained by the trend with Eddington ratio. The radio-loudest quasars have systematically larger variability amplitudes by about 30%, when corrected for the other observed trends, while the distribution of their characteristic timescale is indistinguishable from that of the full sample. We do not detect any statistically robust differences in the characteristic timescale and variability amplitude between the full sample and the small subsample of quasars detected by ROSAT. Our results provide a simple quantitative framework for generating mock quasar light curves, such as currently used in LSST image simulations. C1 [MacLeod, C. L.; Ivezic, Z.; Bullock, E.; Kimball, A.; Sesar, B.; Westman, D.; Brooks, K.; Gibson, R.; Becker, A. C.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Kochanek, C. S.; Kozlowski, S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Kochanek, C. S.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Kelly, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Westman, D.] James Cook Univ, Ctr Astron, Townsville, Qld 4811, Australia. [de Vries, W. H.] Univ Calif Davis, Davis, CA 95616 USA. RP MacLeod, CL (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. EM cmacleod@astro.washington.edu RI Kozlowski, Szymon/G-4799-2013 OI Kozlowski, Szymon/0000-0003-4084-880X FU NSF [AST-0807500, AST-0551161, AST-0708082]; NASA [HF-51243.01, NAS 5-26555, AR9-0015X, AR0-11014X]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; The Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington FX We acknowledge support by NSF grant AST-0807500 to the University of Washington, and NSF grant AST-0551161 to LSST for design and development activity. C. S. K. and S. K. acknowledge support by NSF grant AST-0708082. B. K. acknowledges support by NASA through Hubble Fellowship grant HF-51243.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. R. R. G. gratefully acknowledges support from NASA Chandra grants AR9-0015X and AR0-11014X. We thank an anonymous referee for valuable suggestions regarding the analysis in Section 4.4.; Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www. sdss.org/.; The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 79 TC 158 Z9 158 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2010 VL 721 IS 2 BP 1014 EP 1033 DI 10.1088/0004-637X/721/2/1014 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TP UT WOS:000282193600008 ER PT J AU Li, ZY Spitler, LR Jones, C Forman, WR Kraft, RP Di Stefano, R Tang, SK Wang, QD Gilfanov, M Revnivtsev, M AF Li, Zhiyuan Spitler, Lee R. Jones, Christine Forman, William R. Kraft, Ralph P. Di Stefano, Rosanne Tang, Shikui Wang, Q. Daniel Gilfanov, Marat Revnivtsev, Mikhail TI X-RAY EMISSION FROM THE SOMBRERO GALAXY: DISCRETE SOURCES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (M104); galaxies: spiral; X-rays: binaries; X-rays: galaxies ID CHANDRA MONITORING OBSERVATIONS; GLOBULAR-CLUSTER SYSTEMS; POINT-SOURCE POPULATION; ELLIPTIC GALAXIES; DEEP CHANDRA; BLACK-HOLES; CENTAURUS-A; MASS; BINARIES; FIELD AB We present a study of discrete X-ray sources in and around the bulge-dominated, massive Sa galaxy, Sombrero (M104), based on new and archival Chandra observations with a total exposure of similar to 200 ks. With a detection limit of L(X) approximate to 10(37) erg s(-1) and a field of view covering a galactocentric radius of similar to 30 kpc (11.'5), 383 sources are detected. Cross-correlation with Spitler et al.'s catalog of Sombrero globular clusters (GCs) identified from HST/ACS observations reveals 41 X-ray sources in GCs, presumably low-mass X-ray binaries (LMXBs). Metal-rich GCs are found to have a higher probability of hosting these LMXBs, a trend similar to that found in elliptical galaxies. On the other hand, the four most luminous GC LMXBs, with apparently super-Eddington luminosities for an accreting neutron star, are found in metal-poor GCs. We quantify the differential luminosity functions (LFs) for both the detected GC and field LMXBs, whose power-law indices (similar to 1.1 for the GC-LF and similar to 1.6 for field-LF) are consistent with previous studies for elliptical galaxies. With precise sky positions of the GCs without a detected X-ray source, we further quantify, through a fluctuation analysis, the GC-LF at fainter luminosities down to 1035 erg s-1. The derived index rules out a faint-end slope flatter than 1.1 at a 2 sigma significance, contrary to recent findings in several elliptical galaxies and the bulge of M31. On the other hand, the 2-6 keV unresolved emission places a tight constraint on the field LF, implying a flattened index of similar to 1.0 below 10(37) erg s(-1). We also detect 101 sources in the halo of Sombrero. The presence of these sources cannot be interpreted as galactic LMXBs whose spatial distribution empirically follows the starlight. Their number is also higher than the expected number of cosmic active galactic nuclei (52 +/- 11 [sigma s]) whose surface density is constrained by deep X-ray surveys. We suggest that either the cosmic X-ray background is unusually high in the direction of Sombrero, or a distinct population of X-ray sources is present in the halo of Sombrero. C1 [Li, Zhiyuan; Jones, Christine; Forman, William R.; Kraft, Ralph P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Spitler, Lee R.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Tang, Shikui; Wang, Q. Daniel] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Gilfanov, Marat] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Revnivtsev, Mikhail] Tech Univ Munich, Excellence Cluster Univ, D-85748 Garching, Germany. [Revnivtsev, Mikhail] Russian Acad Sci, Inst Space Res, Moscow 117997, Russia. RP Li, ZY (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM zyli@cfa.harvard.edu RI Tang, Shikui/D-9798-2012; Spitler, Lee/A-9867-2013 OI Spitler, Lee/0000-0001-5185-9876 FU SAO [G08-9088] FX We are grateful to Ryan Hickox for his advice on the fluctuation analysis. This work is supported by the SAO grant G08-9088. NR 50 TC 9 Z9 9 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2010 VL 721 IS 2 BP 1368 EP 1382 DI 10.1088/0004-637X/721/2/1368 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TP UT WOS:000282193600035 ER PT J AU Buemi, CS Umana, G Trigilio, C Leto, P Hora, JL AF Buemi, C. S. Umana, G. Trigilio, C. Leto, P. Hora, J. L. TI VISIR/VLT AND VLA JOINT IMAGING ANALYSIS OF THE CIRCUMSTELLAR NEBULA AROUND IRAS 18576+0341 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; stars: early-type; stars: individual (IRAS 18576+0341); stars: winds, outflows ID LUMINOUS-BLUE-VARIABLES; GALACTIC-CENTER QUINTUPLET; SPITZER-SPACE-TELESCOPE; PLANETARY-NEBULAE; STELLAR WINDS; MASSIVE STARS; IRAS-18576+0341; POPULATION; EMISSION; CARINAE AB High spatial and sensitivity images of the Luminous Blue Variable IRAS 18576+0341 were obtained using the mid-infrared imager VISIR at the Very Large Telescope and the Very Large Array interferometer. The resulting mid-infrared continuum maps show a similar clumpy and approximately circular symmetric nebula, which contrasts sharply with the asymmetry that characterizes the ionized component of the envelope, as evidenced from the radio and [Ne II] line images obtained with comparable spatial resolution. In particular, there is excellent overall agreement between the 12.8 mu m map and the radio images, consistent with free-free emission from circumstellar ionized material surrounding a central stellar wind. The color temperature and optical depth maps obtained from mid-infrared images show only slight fluctuations, suggesting quite uniform dust characteristics over the dust shell. We explore various possibilities to understand the cause of the different morphology of the dusty and gaseous component of the circumstellar envelope which are compatible with the observations. C1 [Buemi, C. S.; Umana, G.; Trigilio, C.; Leto, P.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy. [Hora, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Buemi, CS (reprint author), INAF Osservatorio Astrofis Catania, Via S Sofia 75, I-95123 Catania, Italy. OI Buemi, Carla Simona/0000-0002-7288-4613; Leto, Paolo/0000-0003-4864-2806; Hora, Joseph/0000-0002-5599-4650 FU ASI [I/038/08/0]; PRIN-INAF FX We acknowledge partial financial support from the ASI contract I/038/08/0 "HI-GAL" and from PRIN-INAF 2007. NR 32 TC 7 Z9 7 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2010 VL 721 IS 2 BP 1404 EP 1411 DI 10.1088/0004-637X/721/2/1404 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TP UT WOS:000282193600038 ER PT J AU Abdo, AA Ackermann, M Agudo, I Ajello, M Allafort, A Aller, HD Aller, MF Antolini, E Arkharov, AA Axelsson, M Bach, U Baldini, L Ballet, J Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Berdyugin, A Berenji, B Blandford, RD Blinov, DA Bloom, ED Boettcher, M Bonamente, E Borgland, AW Bouvier, A Bregeon, J Brez, A Brigida, M Bruel, P Buehler, R Buemi, CS Burnett, TH Buson, S Caliandro, GA Cameron, RA Caraveo, PA Carosati, D Carrigan, S Casandjian, JM Cavazzuti, E Cecchi, C Celik, O Chekhtman, A Chen, WP Cheung, CC Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Corbel, S Costamante, L Dermer, CD de Angelis, A de Palma, F Donato, D Silva, EDE Drell, PS Dubois, R Dumora, D Farnier, C Favuzzi, C Fegan, SJ Ferrara, EC Focke, WB Forne, E Fortin, P Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giebels, B Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grove, JE Guiriec, S Gurwell, MA Gusbar, C Gomez, JL Hadasch, D Hagen-Thorn, VA Hayashida, M Hays, E Horan, D Hughes, RE Johannesson, G Johnson, AS Johnson, WN Kamae, T Katagiri, H Kataoka, J Kawai, N Kimeridze, G Knodlseder, J Konstantinova, TS Kopatskaya, EN Koptelova, E Kovalev, YY Kurtanidze, OM Kuss, M Lahteenmaki, A Lande, J Larionov, VM Larionova, EG Larionova, LV Larsson, S Latronico, L Lee, SH Leto, P Lister, ML Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Madejski, GM Makeev, A Massaro, E Mazziotta, MN McConville, W McEnery, JE McHardy, IM Michelson, PF Mitthumsiri, W Mizuno, T Moiseev, AA Monte, C Monzani, ME Morozova, DA Morselli, A Moskalenko, IV Murgia, S Naumann-Godo, M Nikolashvili, MG Nolan, PL Norris, JP Nuss, E Ohno, M Ohsugi, T Okumura, A Omodei, N Orlando, E Ormes, JF Ozaki, M Paneque, D Panetta, JH Parent, D Pasanen, M Pelassa, V Pepe, M Pesce-Rollins, M Piron, F Porter, TA Pushkarev, AB Raino, S Raiteri, CM Rando, R Razzano, M Reimer, A Reimer, O Reinthal, R Ripken, J Ritz, S Roca-Sogorb, M Rodriguez, AY Roth, M Roustazadeh, P Ryde, F Sadrozinski, HFW Sander, A Scargle, JD Sgro, C Sigua, LA Smith, PD Sokolovsky, K Spandre, G Spinelli, P Starck, JL Strickman, MS Suson, DJ Takahashi, H Takahashi, T Takalo, LO Tanaka, T Taylor, B Thayer, JB Thayer, JG Thompson, DJ Tibaldo, L Tornikoski, M Torres, DF Tosti, G Tramacere, A Trigilio, C Troitsky, IS Umana, G Usher, TL Vandenbroucke, J Vasileiou, V Vilchez, N Villata, M Vitale, V Waite, AP Wang, P Winer, BL Wood, KS Yang, Z Ylinen, T Ziegler, M AF Abdo, A. A. Ackermann, M. Agudo, I. Ajello, M. Allafort, A. Aller, H. D. Aller, M. F. Antolini, E. Arkharov, A. A. Axelsson, M. Bach, U. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Berdyugin, A. Berenji, B. Blandford, R. D. Blinov, D. A. Bloom, E. D. Boettcher, M. Bonamente, E. Borgland, A. W. Bouvier, A. Bregeon, J. Brez, A. Brigida, M. Bruel, P. Buehler, R. Buemi, C. S. Burnett, T. H. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Carosati, D. Carrigan, S. Casandjian, J. M. Cavazzuti, E. Cecchi, C. Celik, Oe Chekhtman, A. Chen, W. P. Cheung, C. C. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Corbel, S. Costamante, L. Dermer, C. D. de Angelis, A. de Palma, F. Donato, D. do Couto e Silva, E. Drell, P. S. Dubois, R. Dumora, D. Farnier, C. Favuzzi, C. Fegan, S. J. Ferrara, E. C. Focke, W. B. Forne, E. Fortin, P. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giebels, B. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grove, J. E. Guiriec, S. Gurwell, M. A. Gusbar, C. Gomez, J. L. Hadasch, D. Hagen-Thorn, V. A. Hayashida, M. Hays, E. Horan, D. Hughes, R. E. Johannesson, G. Johnson, A. S. Johnson, W. N. Kamae, T. Katagiri, H. Kataoka, J. Kawai, N. Kimeridze, G. Knoedlseder, J. Konstantinova, T. S. Kopatskaya, E. N. Koptelova, E. Kovalev, Y. Y. Kurtanidze, O. M. Kuss, M. Lahteenmaki, A. Lande, J. Larionov, V. M. Larionova, E. G. Larionova, L. V. Larsson, S. Latronico, L. Lee, S. -H. Leto, P. Lister, M. L. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Madejski, G. M. Makeev, A. Massaro, E. Mazziotta, M. N. McConville, W. McEnery, J. E. McHardy, I. M. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Morozova, D. A. Morselli, A. Moskalenko, I. V. Murgia, S. Naumann-Godo, M. Nikolashvili, M. G. Nolan, P. L. Norris, J. P. Nuss, E. Ohno, M. Ohsugi, T. Okumura, A. Omodei, N. Orlando, E. Ormes, J. F. Ozaki, M. Paneque, D. Panetta, J. H. Parent, D. Pasanen, M. Pelassa, V. Pepe, M. Pesce-Rollins, M. Piron, F. Porter, T. A. Pushkarev, A. B. Raino, S. Raiteri, C. M. Rando, R. Razzano, M. Reimer, A. Reimer, O. Reinthal, R. Ripken, J. Ritz, S. Roca-Sogorb, M. Rodriguez, A. Y. Roth, M. Roustazadeh, P. Ryde, F. Sadrozinski, H. F. -W. Sander, A. Scargle, J. D. Sgro, C. Sigua, L. A. Smith, P. D. Sokolovsky, K. Spandre, G. Spinelli, P. Starck, J. -L. Strickman, M. S. Suson, D. J. Takahashi, H. Takahashi, T. Takalo, L. O. Tanaka, T. Taylor, B. Thayer, J. B. Thayer, J. G. Thompson, D. J. Tibaldo, L. Tornikoski, M. Torres, D. F. Tosti, G. Tramacere, A. Trigilio, C. Troitsky, I. S. Umana, G. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vilchez, N. Villata, M. Vitale, V. Waite, A. P. Wang, P. Winer, B. L. Wood, K. S. Yang, Z. Ylinen, T. Ziegler, M. TI FERMI LARGE AREA TELESCOPE AND MULTI-WAVELENGTH OBSERVATIONS OF THE FLARING ACTIVITY OF PKS 1510-089 BETWEEN 2008 SEPTEMBER AND 2009 JUNE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: jets; gamma rays: galaxies; quasars: individual (PKS 1510-089) ID GAMMA-RAY EMISSION; GALACTIC NUCLEI; X-RAY; SPECTRAL PROPERTIES; RELATIVISTIC JET; COMPLETE SAMPLE; RADIO-SOURCES; EGRET DATA; 3C 454.3; BLAZAR AB We report on the multi-wavelength observations of PKS 1510-089 (a flat spectrum radio quasar (FSRQ) at z = 0.361) during its high activity period between 2008 September and 2009 June. During this 11 month period, the source was characterized by a complex variability at optical, UV, and gamma-ray bands, on timescales down to 6-12 hr. The brightest gamma-ray isotropic luminosity, recorded on 2009 March 26, was similar or equal to 2 x 1048 erg s-1. The spectrum in the Fermi Large Area Telescope energy range shows a mild curvature described well by a log-parabolic law, and can be understood as due to the Klein-Nishina effect. The. -ray flux has a complex correlation with the other wavelengths. There is no correlation at all with the X-ray band, a weak correlation with the UV, and a significant correlation with the optical flux. The. -ray flux seems to lead the optical one by about 13 days. From the UV photometry, we estimated a black hole mass of similar or equal to 5.4 x 10(8)M(circle dot) and an accretion rate of similar or equal to 0.5M(circle dot) yr(-1). Although the power in the thermal and non-thermal outputs is smaller compared to the very luminous and distant FSRQs, PKS 1510-089 exhibits a quite large Compton dominance and a prominent big blue bump (BBB) as observed in the most powerful gamma-ray quasars. The BBB was still prominent during the historical maximum optical state in 2009 May, but the optical/ UV spectral index was softer than in the quiescent state. This seems to indicate that the BBB was not completely dominated by the synchrotron emission during the highest optical state. We model the broadband spectrum assuming a leptonic scenario in which the inverse Compton emission is dominated by the scattering of soft photons produced externally to the jet. The resulting model-dependent jet energetic content is compatible with a scenario in which the jet is powered by the accretion disk, with a total efficiency within the Kerr black hole limit. C1 [Abdo, A. A.; Chekhtman, A.; Cheung, C. C.; Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Parent, D.; Strickman, M. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Abdo, A. A.; Cheung, C. C.] Natl Acad Sci, Washington, DC 20001 USA. [Ackermann, M.; Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bouvier, A.; Buehler, R.; Cameron, R. A.; Chiang, J.; Claus, R.; Costamante, L.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Usher, T. L.; Vandenbroucke, J.; Waite, A. P.; Wang, P.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Ackermann, M.; Ajello, M.; Allafort, A.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Bouvier, A.; Buehler, R.; Cameron, R. A.; Chiang, J.; Claus, R.; Costamante, L.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Lande, J.; Lee, S. -H.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Usher, T. L.; Vandenbroucke, J.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Agudo, I.; Gomez, J. L.; Roca-Sogorb, M.] CSIC, Inst Astrofis Andalucia, Granada 18080, Spain. [Agudo, I.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Aller, H. D.; Aller, M. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Antolini, E.; Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Pepe, M.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Antolini, E.; Bonamente, E.; Cecchi, C.; Ciprini, S.; Germani, S.; Lubrano, P.; Pepe, M.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Arkharov, A. A.; Larionov, V. M.; Pushkarev, A. B.] Pulkovo Observ, St Petersburg 196140, Russia. [Axelsson, M.; Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Axelsson, M.] Lund Observ, SE-22100 Lund, Sweden. [Axelsson, M.; Conrad, J.; Larsson, S.; Ripken, J.; Ryde, F.; Yang, Z.; Ylinen, T.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Bach, U.; Kovalev, Y. Y.; Pushkarev, A. B.; Sokolovsky, K.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Brez, A.; Kuss, M.; Latronico, L.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Casandjian, J. M.; Corbel, S.; Grenier, I. A.; Naumann-Godo, M.; Starck, J. -L.; Tibaldo, L.] Univ Paris Diderot, Lab AIM, CEA IRFU, CNRS,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Rando, R.; Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Carrigan, S.; Rando, R.; Tibaldo, L.] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Berdyugin, A.; Pasanen, M.; Reinthal, R.; Takalo, L. O.] Univ Turku, Tuorla Observ, FI-21500 Piikkio, Finland. [Blinov, D. A.; Hagen-Thorn, V. A.; Konstantinova, T. S.; Kopatskaya, E. N.; Larionov, V. M.; Larionova, E. G.; Larionova, L. V.; Morozova, D. A.; Nikolashvili, M. G.; Troitsky, I. S.] St Petersburg State Univ, Astron Inst, St Petersburg, Russia. [Boettcher, M.; Gusbar, C.; Roustazadeh, P.] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.; Fortin, P.; Giebels, B.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Buemi, C. S.; Leto, P.; Trigilio, C.; Umana, G.] Osserv Astrofis Catania, I-95123 Catania, Italy. [Burnett, T. H.; Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Caliandro, G. A.; Rodriguez, A. Y.; Torres, D. F.] Inst Ciencies Espai IEEC CSIC, Barcelona 08193, Spain. [Caraveo, P. A.] Ist Astrofis Spaziale & Fis Cosm, INAF, I-20133 Milan, Italy. [Carosati, D.] EPT Observ, Tijarafe, La Palma, Spain. [Cavazzuti, E.; Gasparrini, D.] Agenzia Spaziale Italiana ASI, Sci Data Ctr, I-00044 Frascati, Italy. [Celik, Oe; Donato, D.; Ferrara, E. C.; Gehrels, N.; Hays, E.; McConville, W.; McEnery, J. E.; Thompson, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Celik, Oe; Moiseev, A. A.; Vasileiou, V.] NASA, CRESST, Greenbelt, MD 20771 USA. [Celik, Oe; Moiseev, A. A.; Vasileiou, V.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Celik, Oe; Vasileiou, V.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Celik, Oe; Vasileiou, V.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Chekhtman, A.; Makeev, A.; Parent, D.] George Mason Univ, Fairfax, VA 22030 USA. [Chen, W. P.; Koptelova, E.] Natl Cent Univ, Grad Inst Astron, Chungli 32054, Taiwan. [Cohen-Tanugi, J.; Farnier, C.; Nuss, E.; Pelassa, V.; Piron, F.] Univ Montpellier 2, Lab Phys Theor & Astroparticules, CNRS, IN2P3, Montpellier, France. [Conrad, J.; Larsson, S.; Ripken, J.; Yang, Z.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Corbel, S.] Inst Univ France, F-75005 Paris, France. [de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy. [Dumora, D.; Lott, B.] CEN Bordeaux Gradignan, CNRS, IN2P3, UMR 5797, F-33175 Gradignan, France. [Dumora, D.; Lott, B.] Univ Bordeaux, CEN Bordeaux Gradignan, UMR 5797, F-33175 Gradignan, France. [Forne, E.] Agrupaci Astron Sabadell, Sabadell 08206, Spain. [Fukazawa, Y.; Katagiri, H.; Mizuno, T.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Giroletti, M.] Ist Radioastron, INAF, I-40129 Bologna, Italy. [Guiriec, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hadasch, D.; Torres, D. F.] ICREA, Barcelona, Spain. [Hagen-Thorn, V. A.; Larionov, V. M.] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia. [Hughes, R. E.; Sander, A.; Smith, P. D.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA. [Kataoka, J.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Kawai, N.] Tokyo Inst Technol, Dept Phys, Meguro, Tokyo 1528551, Japan. [Kawai, N.] Inst Phys & Chem Res RIKEN, Cosm Radiat Lab, Saitama 3510198, Japan. [Kimeridze, G.; Kurtanidze, O. M.; Sigua, L. A.] Abastumani Observ, GE-0301 Abastumani, Rep of Georgia. [Knoedlseder, J.; Vilchez, N.] Ctr Etud Spatiale Rayonnements, CNRS, UPS, F-31028 Toulouse 4, France. [Kovalev, Y. Y.; Sokolovsky, K.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117810, Russia. [Lahteenmaki, A.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, FIN-02540 Kylmala, Finland. [Lister, M. L.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Massaro, E.] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy. [McConville, W.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McConville, W.; McEnery, J. E.; Moiseev, A. A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [McHardy, I. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Norris, J. P.; Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Ohno, M.; Okumura, A.; Ozaki, M.; Takahashi, T.] Inst Space & Astronaut Sci, JAXA, Kanagawa 2298510, Japan. [Ohsugi, T.; Takahashi, H.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Orlando, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Pushkarev, A. B.] Crimean Astrophys Observ, UA-98409 Nauchnyi, Ukraine. [Raiteri, C. M.; Villata, M.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Ritz, S.; Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Ritz, S.; Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Ryde, F.; Ylinen, T.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Taylor, B.] Lowell Observ, Flagstaff, AZ 86001 USA. [Tramacere, A.] Consorzio Interuniversitario Fis Spaziale CIFS, I-10133 Turin, Italy. [Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Ylinen, T.] Univ Kalmar, Sch Pure & Appl Nat Sci, SE-39182 Kalmar, Sweden. RP Abdo, AA (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. EM enrico.massaro@uniroma1.it RI Grishina, Tatiana/H-6873-2013; Hagen-Thorn, Vladimir/H-3983-2013; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; Pushkarev, Alexander/M-9997-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Blinov, Dmitry/G-9925-2013; Ozaki, Masanobu/K-1165-2013; Rando, Riccardo/M-7179-2013; Kovalev, Yuri/J-5671-2013; Lahteenmaki, Anne/L-5987-2013; Hays, Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Kurtanidze, Omar/J-6237-2014; Funk, Stefan/B-7629-2015; Sokolovsky, Kirill/D-2246-2015; Agudo, Ivan/G-1701-2015; Morozova, Daria/H-1298-2013; Troitskiy, Ivan/K-7979-2013; Starck, Jean-Luc/D-9467-2011; Thompson, David/D-2939-2012; Gehrels, Neil/D-2971-2012; McEnery, Julie/D-6612-2012; Baldini, Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Larionov, Valeri/H-1349-2013; Kopatskaya, Evgenia/H-4720-2013; Larionova, Elena/H-7287-2013 OI Berenji, Bijan/0000-0002-4551-772X; Gasparrini, Dario/0000-0002-5064-9495; Tramacere, Andrea/0000-0002-8186-3793; Baldini, Luca/0000-0002-9785-7726; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Pesce-Rollins, Melissa/0000-0003-1790-8018; Axelsson, Magnus/0000-0003-4378-8785; Giroletti, Marcello/0000-0002-8657-8852; Villata, Massimo/0000-0003-1743-6946; Giordano, Francesco/0000-0002-8651-2394; Larionova, Liudmila/0000-0002-0274-1481; De Angelis, Alessandro/0000-0002-3288-2517; Caraveo, Patrizia/0000-0003-2478-8018; Leto, Paolo/0000-0003-4864-2806; Sgro', Carmelo/0000-0001-5676-6214; Rando, Riccardo/0000-0001-6992-818X; Raiteri, Claudia Maria/0000-0003-1784-2784; Grishina, Tatiana/0000-0002-3953-6676; Hagen-Thorn, Vladimir/0000-0002-6431-8590; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; Buemi, Carla Simona/0000-0002-7288-4613; Blinov, Dmitry/0000-0003-0611-5784; Kovalev, Yuri/0000-0001-9303-3263; Funk, Stefan/0000-0002-2012-0080; Sokolovsky, Kirill/0000-0001-5991-6863; Agudo, Ivan/0000-0002-3777-6182; Morozova, Daria/0000-0002-9407-7804; Troitskiy, Ivan/0000-0002-4218-0148; Starck, Jean-Luc/0000-0003-2177-7794; Thompson, David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888; Reimer, Olaf/0000-0001-6953-1385; Larionov, Valeri/0000-0002-4640-4356; Kopatskaya, Evgenia/0000-0001-9518-337X; Larionova, Elena/0000-0002-2471-6500 FU Russian Foundation for Basic Research [08- 0200545] FX The Lebedev Physical Institute team was partly supported by the Russian Foundation for Basic Research (project 08- 0200545). K. S. was supported by stipend from the IMPRS for Astronomy and Astrophysics. We thank A. P. Marscher and S. Jorstad for providing multi- wavelength data. NR 78 TC 57 Z9 57 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2010 VL 721 IS 2 BP 1425 EP 1447 DI 10.1088/0004-637X/721/2/1425 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TP UT WOS:000282193600041 ER PT J AU Kim, DW Fabbiano, G AF Kim, Dong-Woo Fabbiano, Giuseppina TI X-RAY PROPERTIES OF YOUNG EARLY-TYPE GALAXIES. I. X-RAY LUMINOSITY FUNCTION OF LOW-MASS X-RAY BINARIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; X-rays: binaries; X-rays: galaxies ID CHANDRA MULTIWAVELENGTH PROJECT; GLOBULAR-CLUSTER CONNECTION; NGC-1316 FORNAX-A; ELLIPTIC GALAXIES; POINT-SOURCE; VIRGO CLUSTER; DEEP CHANDRA; MONITORING OBSERVATIONS; STELLAR POPULATIONS; SAURON PROJECT AB We have compared the combined X-ray luminosity function (XLF) of low-mass X-ray binaries (LMXBs) detected in Chandra observations of young, post-merger elliptical galaxies with that of typical old elliptical galaxies. We find that the XLF of the "young" sample does not present the prominent high-luminosity break at L(X) > 5 x 10(38) erg s(-1) found in the old elliptical galaxy XLF. The "young" and "old" XLFs differ with a 3 sigma statistical significance (with a probability less than 0.2% that they derive from the same underlying parent distribution). Young elliptical galaxies host a larger fraction of luminous LMXBs (L(X) > 5 x 10(38) erg s(-1)) than old elliptical galaxies and the XLF of the young galaxy sample is intermediate between that of typical old elliptical galaxies and that of star-forming galaxies. This observational evidence may be related to the last major/minor mergers and the associated star formation. C1 [Kim, Dong-Woo; Fabbiano, Giuseppina] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Kim, DW (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. FU Chandra GO [G08-9133X] FX The data analysis was supported by the CXC CIAO software and CALDB. We have used the NASA NED and ADS facilities and extracted archival data from the Chandra archives. This work was supported by the Chandra GO grant G08-9133X (PI: Kim). We thank Tassos Fragos and Vicky Kalogera for interesting conversations. NR 64 TC 33 Z9 33 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2010 VL 721 IS 2 BP 1523 EP 1530 DI 10.1088/0004-637X/721/2/1523 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TP UT WOS:000282193600048 ER PT J AU Reeves, KK Linker, JA Mikic, Z Forbes, TG AF Reeves, Katharine K. Linker, Jon A. Mikic, Zoran Forbes, Terry G. TI CURRENT SHEET ENERGETICS, FLARE EMISSIONS, AND ENERGY PARTITION IN A SIMULATED SOLAR ERUPTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic reconnection; magnetohydrodynamics (MHD); Sun: coronal mass ejections (CMEs) Sun: flares ID CORONAL MASS EJECTIONS; X-RAY TELESCOPE; FIELD LINE SHRINKAGE; WHOLE SUN MONTH; MAGNETIC RECONNECTION; HELMET STREAMER; 3 DIMENSIONS; FLUX ROPES; MODEL; DISRUPTION AB We investigate coronal energy flow during a simulated coronal mass ejection (CME). We model the CME in the context of the global corona using a 2.5D numerical MHD code in spherical coordinates that includes coronal heating, thermal conduction, and radiative cooling in the energy equation. The simulation domain extends from 1 to 20 Rs. To our knowledge, this is the first attempt to apply detailed energy diagnostics in a flare/ CMEsimulationwhen these important terms are considered in the context of the MHD equations. We find that the energy conservation properties of the code are quite good, conserving energy to within 4% for the entire simulation (more than 6 days of real time). We examine the energy release in the current sheet as the eruption takes place, and find, as expected, that the Poynting flux is the dominant carrier of energy into the current sheet. However, there is a significant flow of energy out of the sides of the current sheet into the upstream region due to thermal conduction along field lines and viscous drag. This energy outflow is spatially partitioned into three separate components, namely, the energy flux flowing out the sides of the current sheet, the energy flowing out the lower tip of the current sheet, and the energy flowing out the upper tip of the current sheet. The energy flow through the lower tip of the current sheet is the energy available for heating of the flare loops. We examine the simulated flare emissions and energetics due to the modeled CME and find reasonable agreement with flare loop morphologies and energy partitioning in observed solar eruptions. The simulation also provides an explanation for coronal dimming during eruptions and predicts that the structures surrounding the current sheet are visible in X-ray observations. C1 [Reeves, Katharine K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Linker, Jon A.; Mikic, Zoran] Predict Sci Inc PSI, San Diego, CA 92121 USA. [Forbes, Terry G.] Univ New Hampshire, Inst Study Earth Oceans & Space EOS, Durham, NH 03824 USA. RP Reeves, KK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kreeves@cfa.harvard.edu; linkerj@predsci.com; mikicz@predsci.com; terry.forbes@unh.edu RI Reeves, Katharine/P-9163-2014 FU NSF-SHINE [ATM0752257] FX K. K. Reeves thanks E. E. DeLuca and H. D. Winter for useful conversations about the numerical simulations. K. R. and T. F. are supported under the NSF-SHINE program, grant number ATM0752257. Additional support for K. R. is provided by NASA grant NNM07AA02C to the Smithsonian Astrophysical Observatory. The work of J. L. and Z. M. is supported by NASA's Heliophysics Theory, LWS, and SR& T Programs, the LWS Strategic Capabilities Program (NASA, NSF, and AFOSR), and the Center for Integrated Space Weather Modeling (an NSF Science and Technology Center). NR 50 TC 48 Z9 48 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2010 VL 721 IS 2 BP 1547 EP 1558 DI 10.1088/0004-637X/721/2/1547 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TP UT WOS:000282193600050 ER PT J AU Brown, PJ Roming, PWA Milne, P Bufano, F Ciardullo, R Elias-Rosa, N Filippenko, AV Foley, RJ Gehrels, N Gronwall, C Hicken, M Holland, ST Hoversten, EA Immler, S Kirshner, RP Li, WD Mazzali, P Phillips, MM Pritchard, T Still, M Turatto, M Vanden Berk, D AF Brown, Peter J. Roming, Peter W. A. Milne, Peter Bufano, Filomena Ciardullo, Robin Elias-Rosa, Nancy Filippenko, Alexei V. Foley, Ryan J. Gehrels, Neil Gronwall, Caryl Hicken, Malcolm Holland, Stephen T. Hoversten, Erik A. Immler, Stefan Kirshner, Robert P. Li, Weidong Mazzali, Paolo Phillips, Mark M. Pritchard, Tyler Still, Martin Turatto, Massimo Vanden Berk, Daniel TI THE ABSOLUTE MAGNITUDES OF TYPE Ia SUPERNOVAE IN THE ULTRAVIOLET SO ASTROPHYSICAL JOURNAL LA English DT Article DE distance scale; dust, extinction; galaxies: distances and redshifts; supernovae: general; ultraviolet: general ID HUBBLE-SPACE-TELESCOPE; SURFACE BRIGHTNESS FLUCTUATIONS; HIGH-REDSHIFT SUPERNOVAE; EARLY-TYPE GALAXIES; LIGHT-CURVE SHAPES; DIGITAL SKY SURVEY; K-CORRECTIONS; DARK ENERGY; DECLINE-RATE; LUMINOSITY INDICATORS AB We examine the absolute magnitudes and light-curve shapes of 14 nearby (redshift z = 0.004-0.027) Type Ia supernovae (SNe Ia) observed in the ultraviolet (UV) with the Swift Ultraviolet/Optical Telescope. Colors and absolute magnitudes are calculated using both a standard Milky Way extinction law and one for the Large Magellanic Cloud that has been modified by circumstellar scattering. We find very different behavior in the near-UV filters (uvw1(rc) covering similar to 2600-3300 (A) over circle after removing optical light, and u approximate to 3000-4000 (A) over circle) compared to a mid-UV filter (uvm2 approximate to 2000-2400 (A) over circle). The uvw1(rc) - b colors show a scatter of similar to 0.3 mag while uvm2-b scatters by nearly 0.9 mag. Similarly, while the scatter in colors between neighboring filters is small in the optical and somewhat larger in the near-UV, the large scatter in the uvm2 - uvw1 colors implies significantly larger spectral variability below 2600 (A) over circle. We find that in the near-UV the absolute magnitudes at peak brightness of normal SNe Ia in our sample are correlated with the optical decay rate with a scatter of 0.4 mag, comparable to that found for the optical in our sample. However, in the mid-UV the scatter is larger, similar to 1 mag, possibly indicating differences in metallicity. We find no strong correlation between either the UV light-curve shapes or the UV colors and the UV absolute magnitudes. With larger samples, the UV luminosity might be useful as an additional constraint to help determine distance, extinction, and metallicity in order to improve the utility of SNe Ia as standardized candles. C1 [Brown, Peter J.; Roming, Peter W. A.; Ciardullo, Robin; Gronwall, Caryl; Hoversten, Erik A.; Pritchard, Tyler] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Milne, Peter] Univ Arizona, Steward Observ, Tucson, AZ 85719 USA. [Bufano, Filomena; Mazzali, Paolo] INAF Osservatorio Astron Padova, I-35122 Padua, Italy. [Elias-Rosa, Nancy] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Filippenko, Alexei V.; Li, Weidong] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Foley, Ryan J.; Hicken, Malcolm; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gehrels, Neil; Holland, Stephen T.; Immler, Stefan] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Holland, Stephen T.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Holland, Stephen T.; Immler, Stefan] NASA GFC, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA. [Immler, Stefan] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mazzali, Paolo] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Mazzali, Paolo] Scuola Normale Super Pisa, I-56126 Pisa, Italy. [Phillips, Mark M.] Las Campanas Observ, La Serena, Chile. [Still, Martin] Univ Coll London, Dept Space & Climate Phys, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Still, Martin] NASA, Ames Res Ctr, Moffett Field, CA 93045 USA. [Turatto, Massimo] Osserv Astrofis Catania, I-95123 Catania, Italy. [Vanden Berk, Daniel] St Vincent Coll, Latrobe, PA 15650 USA. RP Brown, PJ (reprint author), Univ Utah, Dept Phys & Astron, 115 South 1400 East 201, Salt Lake City, UT 84112 USA. EM pbrown@physics.utah.edu RI Gehrels, Neil/D-2971-2012; Elias-Rosa, Nancy/D-3759-2014; OI Elias-Rosa, Nancy/0000-0002-1381-9125; Turatto, Massimo/0000-0002-9719-3157 FU NASA [NAS5-00136, NNH06ZDA001N]; NSF [AST-0908886, NNX09AG54G, AST-0907903]; PRIN of Italian Ministry of University and Science Research [2006022731] FX We are grateful to A. Goobar for extending his circumstellar extinction model into the UV for us. This work is supported at Penn State University by NASA contract NAS5-00136 and Swift Guest Investigator grant NNH06ZDA001N. A.V.F. is grateful for the support of NSF grant AST-0908886 and Swift Guest Investigator grant NNX09AG54G. This work made use of public data in the Swift data archive and the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. The CfA Supernova Program at Harvard University is supported by NSF grant AST-0907903. The work of M.T. is supported by grant no.. 2006022731 of the PRIN of Italian Ministry of University and Science Research. NR 116 TC 53 Z9 53 U1 2 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2010 VL 721 IS 2 BP 1608 EP 1626 DI 10.1088/0004-637X/721/2/1608 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TP UT WOS:000282193600057 ER PT J AU Milne, PA Brown, PJ Roming, PWA Holland, ST Immler, S Filippenko, AV Ganeshalingam, M Li, WD Stritzinger, M Phillips, MM Hicken, M Kirshner, RP Challis, PJ Mazzali, P Schmidt, BP Bufano, F Gehrels, N Vanden Berk, D AF Milne, Peter A. Brown, Peter J. Roming, Peter W. A. Holland, Stephen T. Immler, Stefan Filippenko, Alexei V. Ganeshalingam, Mohan Li, Weidong Stritzinger, Maximilian Phillips, Mark M. Hicken, Malcolm Kirshner, Robert P. Challis, Peter J. Mazzali, Paolo Schmidt, Brian P. Bufano, Filomena Gehrels, Neil Vanden Berk, Daniel TI NEAR-ULTRAVIOLET PROPERTIES OF A LARGE SAMPLE OF TYPE Ia SUPERNOVAE AS OBSERVED WITH THE Swift UVOT SO ASTROPHYSICAL JOURNAL LA English DT Article DE distance scale; dust, extinction; galaxies: distances and redshifts; supernovae: general; ultraviolet: general ID HUBBLE-SPACE-TELESCOPE; ULTRA-VIOLET/OPTICAL TELESCOPE; LIGHT-CURVE SHAPES; X-RAY OBSERVATIONS; II-P SUPERNOVAE; DECLINE-RATE; INFRARED OBSERVATIONS; OPTICAL PHOTOMETRY; IMPROVED DISTANCES; SYNTHETIC SPECTRA AB We present ultraviolet (UV) and optical photometry of 26 Type Ia supernovae (SNe Ia) observed from 2005 March to 2008 March with the NASA Swift Ultraviolet and Optical Telescope (UVOT). The dataset consists of 2133 individual observations, making it by far the most complete study of the UV emission from SNe Ia to date. Grouping the SNe into three subclasses as derived from optical observations, we investigate the evolution of the colors of these SNe, finding a high degree of homogeneity within the normal subclass, but dramatic differences between that group and the subluminous and SN 2002cx-like groups. For the normal events, the redder UV filters on UVOT (u, uvw1) show more homogeneity than do the bluer UV filters (uvm2, uvw2). Searching for purely UV characteristics to determine existing optically based groupings, we find the peak width to be a poor discriminant, but we do see a variation in the time delay between peak emission and the late, flat phase of the light curves. The UV light curves peak a few days before the B band for most subclasses (as was previously reported by Jha et al.), although the SN 2002cx-like objects peak at a very early epoch in the UV. That group also features the bluest emission observed among SNe Ia. As the observational campaign is ongoing, we discuss the critical times to observe, as determined by this study, in order to maximize the scientific output of future observations. C1 [Milne, Peter A.] Univ Arizona, Steward Observ, Tucson, AZ 85719 USA. [Brown, Peter J.; Roming, Peter W. A.; Vanden Berk, Daniel] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Holland, Stephen T.; Immler, Stefan; Bufano, Filomena; Gehrels, Neil] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Holland, Stephen T.; Immler, Stefan] Univ Space Res Assoc, Columbia, MD 21044 USA. [Filippenko, Alexei V.; Ganeshalingam, Mohan; Li, Weidong] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Stritzinger, Maximilian; Phillips, Mark M.] Carnegie Observ, Las Campanas Observ, La Serena, Chile. [Stritzinger, Maximilian] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [Hicken, Malcolm; Kirshner, Robert P.; Challis, Peter J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mazzali, Paolo] Astron Observ Padova, INAF, I-35122 Padua, Italy. [Mazzali, Paolo] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Schmidt, Brian P.] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Observ, Weston, ACT 2611, Australia. [Bufano, Filomena] Univ Padua, Dipartmento Astron, I-35122 Padua, Italy. [Vanden Berk, Daniel] St Vincent Coll, Latrobe, PA USA. RP Milne, PA (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85719 USA. RI Gehrels, Neil/D-2971-2012; OI Schmidt, Brian/0000-0001-6589-1287; stritzinger, maximilian/0000-0002-5571-1833 FU National Science Foundation (NSF) [AST-0607485, AST-0908886, AST-0606772, AST-0907903]; TABASGO Foundation; US Department of Energy [DE-FC02-06ER41453, DE-FG02-08ER41563, NNX09AG54G]; NASA [NAS5-00136]; Sun Microsystems, Inc.; Hewlett-Packard Company; AutoScope Corporation; Lick Observatory; University of California; Sylvia & Jim Katzman Foundation FX We thank the Mission Operations team at Penn State University for scheduling so many UVOT SN Ia observations on short notice. We are grateful to Stephane Blondin for his efforts on behalf of the CfA Supernova Program, and X. Wang for categorization of NHV and NNN SNe Ia. P.A.M. thanks K. Krisciunas for assistance in obtaining information on specific supernovae. The research of A.V.F.'s supernova group at UC Berkeley is supported by National Science Foundation (NSF) grants AST-0607485 and AST-0908886, the TABASGO Foundation, US Department of Energy SciDAC grant DE-FC02-06ER41453, US Department of Energy grant DE-FG02-08ER41563, and Swift Guest Investigator grant NNX09AG54G. The work at PSU is sponsored by NASA contract NAS5-00136. KAIT and its ongoing operations were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, and the TABASGO Foundation. Supernova research at the Harvard College Observatory is supported in part by the NSF through grants AST-0606772 and AST-0907903. NR 96 TC 41 Z9 41 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2010 VL 721 IS 2 BP 1627 EP 1655 DI 10.1088/0004-637X/721/2/1627 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TP UT WOS:000282193600058 ER PT J AU Lanz, L Jones, C Forman, WR Ashby, MLN Kraft, R Hickox, RC AF Lanz, Lauranne Jones, Christine Forman, William R. Ashby, Matthew L. N. Kraft, Ralph Hickox, Ryan C. TI CONSTRAINING THE OUTBURST PROPERTIES OF THE SMBH IN FORNAX A THROUGH X-RAY, INFRARED, AND RADIO OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (NGC 1316); galaxies: structure; infrared: galaxies; radio continuum: galaxies; X-rays: galaxies ID SPITZER-SPACE-TELESCOPE; GALAXY NGC-1316 FORNAX; MULTIBAND IMAGING PHOTOMETER; SUPERMASSIVE BLACK-HOLE; ACTIVE GALACTIC NUCLEI; NEARBY GALAXIES; CENTAURUS-A; ABSOLUTE CALIBRATION; CHANDRA OBSERVATION; ELLIPTIC GALAXIES AB Combined Spitzer, Chandra, XMM-Newton, and VLA observations of the giant radio galaxy NGC 1316 (Fornax A) show a radio jet and X-ray cavities from active galactic nucleus (AGN) outbursts most likely triggered by a merger with a late-type galaxy at least 0.4 Gyr ago. We detect a weak nucleus with a spectral energy distribution typical of a low-luminosity AGN with a bolometric luminosity of 2.4 x 10(42) erg s(-1). We examine the Spitzer IRAC and MIPS images of NGC 1316. We find that the dust emission is strongest in regions with little or no radio emission and that the particularly large infrared luminosity relative to the galaxy's K-band luminosity implies an external origin for the dust. The inferred dust mass implies that the merger spiral galaxy had a stellar mass of (1-6) x 10(10) M(circle dot) and a gas mass of (2-4) x 10(9) M(circle dot). X-ray cavities in the Chandra and XMM-Newton images likely result from the expansion of relativistic plasma ejected by the AGN. The soft (0.5-2.0 keV) Chandra images show a small similar to 15 '' (1.6 kpc) cavity coincident with the radio jet, while the XMM-Newton image shows two large X-ray cavities lying 320 '' (34.8 kpc) east and west of the nucleus, each approximately 230 '' (25 kpc) in radius. Current radio observations do not show emission within these cavities. The radio lobes lie at radii of 14'.3 (93.3 kpc) and 15'.6 (101 kpc), more distant from the nucleus than the detected X-ray cavities. The relative morphology of the large scale 1.4 GHz and X-ray emission suggests they were products of two distinct outbursts, an earlier one creating the radio lobes and a later one producing the X-ray cavities. Alternatively, if a single outburst created both the X-ray cavities and the radio lobes, this would require that the radio morphology is not fully defined by the 1.4 GHz emission. For the more likely two outbursts scenarios, we use the buoyancy rise times to estimate an age for the more recent outburst that created the X-ray cavities of 0.1 Gyr and the PV work done by the expanding plasma that created the X-ray cavities to estimate the outburst's energy to be 10(58) erg. The present size and location of the radio lobes imply that the outburst that created them happened similar to 0.4 Gyr ago and released similar to 5 x 10(58) erg. C1 [Lanz, Lauranne; Jones, Christine; Forman, William R.; Ashby, Matthew L. N.; Kraft, Ralph; Hickox, Ryan C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hickox, Ryan C.] Univ Durham, Dept Phys, Durham DH1 3LE, England. RP Lanz, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM llanz@head.cfa.harvard.edu OI Lanz, Lauranne/0000-0002-3249-8224 FU Smithsonian Institution; Chandra X-ray Center; NASA [NNX07AQ18G] FX We are grateful to C. Horellou and J. H. Black for providing us with CO(2-1) intensities and for their comments regarding the molecular gas kinematics, Zhiyuan Li for his useful discussion on calculating masses, Dharam Lal for his assistance in creating the 4.89 GHz map, and to Ramesh Narayan for his comments. We thank the anonymous referee for the many comments that improved this work. This work was based on archival data obtained from the Spitzer Science Archive, the Chandra Data Archive, and the XMM-Newton Science Data Archive. Archived images were also obtained from the Hubble Legacy Archive, the NASA/IPAC Extragalactic Database, and the National Radio Astronomy Observatory Archive. We thank Z. Levay of the Space Telescope Science Institute for his assistance in obtaining the Hubble ACS image. This work was supported by the Smithsonian Institution, the Chandra X-ray Center, and NASA contract NNX07AQ18G. NR 69 TC 16 Z9 16 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2010 VL 721 IS 2 BP 1702 EP 1713 DI 10.1088/0004-637X/721/2/1702 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TP UT WOS:000282193600063 ER PT J AU Kafka, S Tappert, C Ribeiro, T Honeycutt, RK Hoard, DW Saar, S AF Kafka, S. Tappert, C. Ribeiro, T. Honeycutt, R. K. Hoard, D. W. Saar, S. TI LOW-STATE MAGNETIC STRUCTURES IN POLARS: NATURE OR NURTURE? SO ASTROPHYSICAL JOURNAL LA English DT Article DE novae, cataclysmic variables; stars: individual (BL Hyi, AM Her, ST LMi, VV Pup, EF Eri); stars: magnetic field ID EMISSION-LINE REGIONS; VARIABLE ST-LMI; AM-HERCULIS; CATACLYSMIC VARIABLES; X-RAY; VV-PUPPIS; BL HYI; SLINGSHOT PROMINENCES; ROCHE TOMOGRAPHY; PERIOD GAP AB We present an orbit-resolved study of the magnetic cataclysmic variable (MCV) BL Hyi in its low state, and we explore the origin of its H alpha emission line components, their properties, and their possible formation mechanism. We tentatively associate one of the line components with a high-velocity component also seen in the high state. We propose a scenario in which streaming prominence- like magnetic loops (super-prominences) are kept in place by magnetic field interactions between the white dwarf and the donor star and are responsible for the high-velocity line components in the Balmer lines. We also discuss how this is in accord with the standard scenario of the secular evolution for MCVs. Finally, we offer an observational test of our ideas and present challenges for future theoretical studies. C1 [Kafka, S.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. [Kafka, S.; Hoard, D. W.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Tappert, C.] Univ Valparaiso, Dept Fis & Astrofis, Valparaiso, Chile. [Ribeiro, T.] Univ Fed Santa Catarina, Dept Fis, BR-88040900 Florianopolis, SC, Brazil. [Honeycutt, R. K.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. [Saar, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kafka, S (reprint author), Carnegie Inst Washington, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. EM skafka@dtm.ciw.edu OI Hoard, Donald W./0000-0002-6800-6519 NR 54 TC 5 Z9 5 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2010 VL 721 IS 2 BP 1714 EP 1724 DI 10.1088/0004-637X/721/2/1714 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TP UT WOS:000282193600064 ER PT J AU Agol, E Cowan, NB Knutson, HA Deming, D Steffen, JH Henry, GW Charbonneau, D AF Agol, Eric Cowan, Nicolas B. Knutson, Heather A. Deming, Drake Steffen, Jason H. Henry, Gregory W. Charbonneau, David TI THE CLIMATE OF HD 189733b FROM FOURTEEN TRANSITS AND ECLIPSES MEASURED BY SPITZER SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems ID HUBBLE-SPACE-TELESCOPE; HOT SUPER-EARTHS; EXTRASOLAR PLANET; ATMOSPHERIC CIRCULATION; TRANSMISSION SPECTRUM; INFRARED-EMISSION; TIMING VARIATIONS; SYSTEM HD-189733; ROTATION PERIOD; LIGHT CURVES AB We present observations of six transits and six eclipses of the transiting planet system HD 189733 taken with the Spitzer Space Telescope's Infrared Array Camera (IRAC) at 8 mu m, as well as a re-analysis of previously published data. We use several novel techniques in our data analysis, the most important of which is a new correction for the detector "ramp" variation with a double-exponential function, which performs better and is a better physical model for this detector variation. Our main scientific findings are (1) an upper limit on the variability of the dayside planet flux of 2.7% (68% confidence); (2) the most precise set of transit times measured for a transiting planet, with an average accuracy of 3 s; (3) a lack of transit-timing variations, excluding the presence of second planets in this system above 20% of the mass of Mars in low-order mean-motion resonance at 95% confidence; (4) a confirmation of the planet's phase variation, finding the night side is 64% as bright as the day side, as well as an upper limit on the nightside variability of 17% (68% confidence); (5) a better correction for stellar variability at 8 mu m causing the phase function to peak 3.5 hr before secondary eclipse, confirming that the advection and radiation timescales are comparable at the 8 mu m photosphere; (6) variation in the depth of transit, which possibly implies variations in the surface brightness of the portion of the star occulted by the planet, posing a fundamental limit on non-simultaneous multi-wavelength transit absorption measurements of planet atmospheres; (7) a measurement of the infrared limb darkening of the star, which is in good agreement with stellar atmosphere models; (8) an offset in the times of secondary eclipse of 69 s, which is mostly accounted for by a 31 s light-travel time delay and 33 s delay due to the shift of ingress and egress by the planet hot spot; this confirms that the phase variation is due to an offset hot spot on the planet; (9) a retraction of the claimed eccentricity of this system due to the offset of secondary eclipse, which is now just an upper limit; and (10) high-precision measurements of the parameters of this system. These results were enabled by the exquisite photometric precision of Spitzer IRAC; for repeat observations the scatter is less than 0.35 mmag over the 590 day timescale of our observations after decorrelating with detector parameters. C1 [Agol, Eric; Cowan, Nicolas B.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Agol, Eric] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93110 USA. [Agol, Eric] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93110 USA. [Knutson, Heather A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Deming, Drake] NASA, Goddard Space Flight Ctr, Planetary Syst Lab, Greenbelt, MD 20771 USA. [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Henry, Gregory W.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. [Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Agol, E (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. RI Steffen, Jason/A-4320-2013; Agol, Eric/B-8775-2013; OI Agol, Eric/0000-0002-0802-9145; Charbonneau, David/0000-0002-9003-484X FU NASA; Miller Institute for Basic Research in Science; National Science Foundation [NSF PHY05-51164, 0645416] FX This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory (JPL), California Institute of Technology under contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. E.A. acknowledges the hospitality of the Institute for Theory and Computation at the Harvard-Smithsonian Center for Astrophysics, the Michigan Center for Theoretical Physics, and the Kavli Institute for Theoretical Physics where portions of this work were completed. H.A.K. is supported by a fellowship from the Miller Institute for Basic Research in Science. This research was supported in part by the National Science Foundation under grant No. NSF PHY05-51164 and CAREER grant No. 0645416. NR 70 TC 125 Z9 125 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2010 VL 721 IS 2 BP 1861 EP 1877 DI 10.1088/0004-637X/721/2/1861 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TP UT WOS:000282193600076 ER PT J AU Acciari, VA Aliu, E Arlen, T Beilicke, M Benbow, W Bottcher, M Bradbury, SM Buckley, JH Bugaev, V Butt, Y Byrum, K Cannon, A Celik, O Cesarini, A Chow, YC Ciupik, L Cogan, P Cui, W Daniel, MK Dickherber, R Ergin, T Falcone, A Fegan, SJ Finley, JP Fortin, P Fortson, L Furniss, A Gall, D Gibbs, K Gillanders, GH Godambe, S Grube, J Guenette, R Gyuk, G Hanna, D Hays, E Holder, J Horan, D Hui, CM Humensky, TB Imran, A Kaaret, P Karlsson, N Kertzman, M Kieda, D Kildea, J Konopelko, A Krawczynski, H Krennrich, F Lang, MJ LeBohec, S Maier, G McCann, A McCutcheon, M Millis, J Moriarty, P Mukherjee, R Nagai, T Ong, RA Otte, AN Pandel, D Perkins, JS Petry, D Pizlo, F Pohl, M Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Rose, HJ Schroedter, M Sembroski, GH Smith, AW Steele, D Swordy, SP Theiling, M Toner, JA Varlotta, A Vassiliev, VV Wagner, RG Wakely, SP Ward, JE Weekes, TC Weinstein, A Williams, DA Wissel, S Wood, M Zitzer, B AF Acciari, V. A. Aliu, E. Arlen, T. Beilicke, M. Benbow, W. Boettcher, M. Bradbury, S. M. Buckley, J. H. Bugaev, V. Butt, Y. Byrum, K. Cannon, A. Celik, O. Cesarini, A. Chow, Y. C. Ciupik, L. Cogan, P. Cui, W. Daniel, M. K. Dickherber, R. Ergin, T. Falcone, A. Fegan, S. J. Finley, J. P. Fortin, P. Fortson, L. Furniss, A. Gall, D. Gibbs, K. Gillanders, G. H. Godambe, S. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Hays, E. Holder, J. Horan, D. Hui, C. M. Humensky, T. B. Imran, A. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Kildea, J. Konopelko, A. Krawczynski, H. Krennrich, F. Lang, M. J. LeBohec, S. Maier, G. McCann, A. McCutcheon, M. Millis, J. Moriarty, P. Mukherjee, R. Nagai, T. Ong, R. A. Otte, A. N. Pandel, D. Perkins, J. S. Petry, D. Pizlo, F. Pohl, M. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Rose, H. J. Schroedter, M. Sembroski, G. H. Smith, A. W. Steele, D. Swordy, S. P. Theiling, M. Toner, J. A. Varlotta, A. Vassiliev, V. V. Wagner, R. G. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Williams, D. A. Wissel, S. Wood, M. Zitzer, B. TI VERITAS OBSERVATIONS OF A VERY HIGH ENERGY gamma-RAY FLARE FROM THE BLAZAR 3C 66A (vol 693, pg L104, 2009) SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Correction C1 [Acciari, V. A.; Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Aliu, E.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Aliu, E.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Arlen, T.; Celik, O.; Chow, Y. C.; Fegan, S. J.; Ong, R. A.; Vassiliev, V. V.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Gibbs, K.; Kildea, J.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Boettcher, M.] Ohio Univ, Inst Astrophys, Dept Phys & Astron, Athens, OH 45701 USA. [Bradbury, S. M.; Daniel, M. K.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Butt, Y.; Ergin, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Byrum, K.; Smith, A. W.; Wagner, R. G.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cannon, A.; Grube, J.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cesarini, A.; Gillanders, G. H.; Lang, M. J.; Toner, J. A.] Natl Univ Ireland, Sch Phys, Galway, Ireland. [Ciupik, L.; Fortson, L.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cogan, P.; Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; McCutcheon, M.; Ragan, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Cui, W.; Finley, J. P.; Gall, D.; Pizlo, F.; Sembroski, G. H.; Varlotta, A.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Fortin, P.; Mukherjee, R.] Columbia Univ, Dept Phys & Astron, Barnard Coll, New York, NY 10027 USA. [Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Godambe, S.; Hui, C. M.; Kieda, D.; LeBohec, S.] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. [Hays, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Horan, D.] Ecole Polytech, CNRS, Lab Leprince Ringuet, IN2P3, F-91128 Palaiseau, France. [Humensky, T. B.; Swordy, S. P.; Wakely, S. P.; Wissel, S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Imran, A.; Krennrich, F.; Nagai, T.; Pohl, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kaaret, P.; Pandel, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA. [Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Petry, D.] European So Observ, D-85748 Garching, Germany. [Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. RP Acciari, VA (reprint author), Galway Mayo Inst Technol, Dept Life & Phys Sci, Dublin Rd, Galway, Ireland. EM jperkins@cfa.harvard.edu RI Hays, Elizabeth/D-3257-2012; Daniel, Michael/A-2903-2010 OI Daniel, Michael/0000-0002-8053-7910 NR 3 TC 2 Z9 2 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2010 VL 721 IS 2 BP L203 EP L204 DI 10.1088/2041-8205/721/2/L203 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TB UT WOS:000282192200027 ER PT J AU Besla, G Kallivayalil, N Hernquist, L van der Marel, RP Cox, TJ Keres, D AF Besla, G. Kallivayalil, N. Hernquist, L. van der Marel, R. P. Cox, T. J. Keres, D. TI SIMULATIONS OF THE MAGELLANIC STREAM IN A FIRST INFALL SCENARIO SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: halos; galaxies: individual (Magellanic Clouds); galaxies: kinematics and dynamics ID HIGH-VELOCITY CLOUDS; N-BODY SIMULATIONS; PROPER MOTION; MILKY-WAY; HI SURVEY; GALAXIES; ORIGIN; HALO; KINEMATICS; SYSTEM AB Recent high-precision proper motions from the Hubble Space Telescope suggest that the Large and Small Magellanic Clouds (LMC and SMC, respectively) are either on their first passage or on an eccentric long period (>6 Gyr) orbit about the Milky Way (MW). This differs markedly from the canonical picture in which the Clouds travel on a quasi-periodic orbit about the MW (period of similar to 2 Gyr). Without a short-period orbit about the MW, the origin of the Magellanic Stream, a young (1-2 Gyr old) coherent stream of H I gas that trails the Clouds similar to 150 degrees across the sky, can no longer be attributed to stripping by MW tides and/or ram pressure stripping by MW halo gas. We propose an alternative formation mechanism in which material is removed by LMC tides acting on the SMC before the system is accreted by the MW. We demonstrate the feasibility and generality of this scenario using an N-body/smoothed particle hydrodynamics simulation with cosmologically motivated initial conditions constrained by the observations. Under these conditions, we demonstrate that it is possible to explain the origin of the Magellanic Stream in a first infall scenario. This picture is generically applicable to any gas-rich dwarf galaxy pair infalling toward a massive host or interacting in isolation. C1 [Besla, G.; Hernquist, L.; Keres, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kallivayalil, N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [van der Marel, R. P.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Cox, T. J.] Carnegie Observ, Pasadena, CA 91101 USA. RP Besla, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gbesla@cfa.harvard.edu NR 49 TC 90 Z9 90 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2010 VL 721 IS 2 BP L97 EP L101 DI 10.1088/2041-8205/721/2/L97 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TB UT WOS:000282192200005 ER PT J AU Cassano, R Ettori, S Giacintucci, S Brunetti, G Markevitch, M Venturi, T Gitti, M AF Cassano, R. Ettori, S. Giacintucci, S. Brunetti, G. Markevitch, M. Venturi, T. Gitti, M. TI ON THE CONNECTION BETWEEN GIANT RADIO HALOS AND CLUSTER MERGERS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: clusters: general; radiation mechanisms: non-thermal; radio continuum: general; X-rays: galaxies: clusters ID GALAXY CLUSTERS; REACCELERATION MODEL; SAMPLE; SUBSTRUCTURE; EVOLUTION; EMISSION; PERSEUS AB The frequently observed association between giant radio halos (RHs) and merging galaxy clusters has driven present theoretical models of non-thermal emission from galaxy clusters, which are based on the idea that the energy dissipated during cluster-cluster mergers could power the formation of RHs. To quantitatively test the merger-halo connection, we present the first statistical study based on deep radio data and X-ray observations of a complete X-ray-selected sample of galaxy clusters with X-ray luminosity >= 5 x 10(44) erg s(-1) and redshift 0.2 <= z <= 0.32. Using several methods to characterize cluster substructures, namely, the power ratios, centroid shift, and X-ray brightness concentration parameter, we show that clusters with and without RH can be quantitatively differentiated in terms of their dynamical properties. In particular, we confirm that RHs are associated with dynamically disturbed clusters and clusters without RH are more "relaxed," with only a couple of exceptions where a disturbed cluster does not exhibit a halo. C1 [Cassano, R.; Giacintucci, S.; Brunetti, G.; Venturi, T.] IRA, INAF, I-40129 Bologna, Italy. [Cassano, R.; Giacintucci, S.; Markevitch, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ettori, S.; Gitti, M.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Ettori, S.] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy. RP Cassano, R (reprint author), IRA, INAF, Via Gobetti 101, I-40129 Bologna, Italy. RI Ettori, Stefano/N-5004-2015; OI Ettori, Stefano/0000-0003-4117-8617; Venturi, Tiziana/0000-0002-8476-6307; Brunetti, Gianfranco/0000-0003-4195-8613; Gitti, Myriam/0000-0002-0843-3009; Cassano, Rossella/0000-0003-4046-0637 FU INAF [PRIN-INAF2007, PRIN-INAF2008]; ASI-INAF [I/088/06/0]; NASA [ARO-11017X, G09-0133X] FX We thank the referee for useful comments. This work was partially supported by INAF under grants PRIN-INAF2007 and PRIN-INAF2008, and by ASI-INAF under grant I/088/06/0. Support was also provided by NASA via Chandra grants ARO-11017X and G09-0133X. R.C. and G.B. thank the Harvard-Smithsonian Center for Astrophysics for its hospitality. NR 28 TC 117 Z9 117 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2010 VL 721 IS 2 BP L82 EP L85 DI 10.1088/2041-8205/721/2/L82 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TB UT WOS:000282192200002 ER PT J AU Currie, T Bailey, V Fabrycky, D Murray-Clay, R Rodigas, T Hinz, P AF Currie, Thayne Bailey, Vanessa Fabrycky, Daniel Murray-Clay, Ruth Rodigas, Timothy Hinz, Phil TI HIGH-CONTRAST 3.8 mu m IMAGING OF THE BROWN DWARF/PLANET-MASS COMPANION TO GJ 758 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE brown dwarfs ID YOUNG SUBSTELLAR COMPANION; EXTRASOLAR GIANT PLANETS; HR 8799; BINARY-SYSTEM; DWARFS; DISCOVERY; STARS; DISK; SUN; AGE AB We present L'-band (3.8 mu m) MMT/Clio high-contrast imaging data for the nearby star GJ 758, which was recently reported by Thalmann et al. to have one-possibly two-faint comoving companions (GJ 758B and "C," respectively). GJ 758B is detected in two distinct data sets. Additionally, we report a possible detection of the object identified by Thalmann et al. as " GJ 758C" in our more sensitive data set, though it is likely a residual speckle. However, if it is the same object as that reported by Thalmann et al. it cannot be a companion in a bound orbit. GJ 758B has an H - L' color redder than nearly all known L-T8 dwarfs. Based on comparisons with the COND evolutionary models, GJ 758B has T(e) similar to 560 K(-90K)(+150K) and a mass ranging from similar to 10-20 M(J) if it is similar to 1 Gyr old to similar to 25-40 M(J) if it is 8.7 Gyr old. GJ 758B is likely in a highly eccentric orbit, e similar to 0.73(-0.21)(+ 0.12), with a semimajor axis of similar to 44AU(-14AU)(+32AU). Though GJ 758B is sometimes discussed within the context of exoplanet direct imaging, its mass is likely greater than the deuterium-burning limit and its formation may resemble that of binary stars rather than that of Jovian-mass planets. C1 [Currie, Thayne] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bailey, Vanessa; Rodigas, Timothy; Hinz, Phil] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Fabrycky, Daniel; Murray-Clay, Ruth] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Currie, T (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. FU NASA; Michelson Fellowship; Institute for Theory and Computation Fellowship FX We thank the anonymous referee and Adam Kraus for suggestions that strengthened this Letter and Adam Burgasser, Marc Kuchner, Scott Kenyon, and Jonathan Irwin for other useful discussions. T.C. is supported by a NASA Postdoctoral Fellowship, D.F. is supported by a Michelson Fellowship, and R.M.-C. is supported by an Institute for Theory and Computation Fellowship. NR 40 TC 15 Z9 15 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2010 VL 721 IS 2 BP L177 EP L181 DI 10.1088/2041-8205/721/2/L177 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TB UT WOS:000282192200022 ER PT J AU Kilic, M Prieto, CA Brown, WR Agueros, MA Kenyon, SJ Camilo, F AF Kilic, Mukremin Prieto, Carlos Allende Brown, Warren R. Agueeros, M. A. Kenyon, S. J. Camilo, Fernando TI ACCURATE MASSES FOR THE PRIMARY AND SECONDARY IN THE ECLIPSING WHITE DWARF BINARY NLTT 11748 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE stars: individual (NLTT 11748); stars: low-mass; white dwarfs ID STARS; DISCOVERY; EVOLUTION; COMPANION; HELIUM AB We measure the radial velocity curve of the eclipsing detached white dwarf binary NLTT 11748. The primary exhibits velocity variations with a semi-amplitude of 273 km s(-1) and an orbital period of 5.641 hr. We do not detect any spectral features from the secondary star or any spectral changes during the secondary eclipse. We use our composite spectrum to constrain the temperature and surface gravity of the primary to be T(eff) = 8690 +/- 140 K and log g = 6.54 +/- 0.05, which correspond to a mass of 0.18 M(circle dot). For an inclination angle of 89 degrees.9 derived from the eclipse modeling, the mass function requires a 0.76 M(circle dot) companion. The merger time for the system is 7.2 Gyr. However, due to the extreme mass ratio of 0.24, the binary will most likely create an AM CVn system instead of a merger. C1 [Kilic, Mukremin; Brown, Warren R.; Kenyon, S. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Prieto, Carlos Allende] Inst Astrofis Canarias, Tenerife 38205, Spain. [Agueeros, M. A.; Camilo, Fernando] Columbia Univ, Dept Astron, New York, NY 10027 USA. RP Kilic, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mkilic@cfa.harvard.edu RI Agueros, Marcel/K-7998-2014; OI Agueros, Marcel/0000-0001-7077-3664; Kenyon, Scott/0000-0003-0214-609X FU NASA; NSF [AST-0602099]; US National Science Foundation; Caltech FX We thank the referee S. Vennes for helpful suggestions, D. Koester for kindly providing WD model spectra, and S. Ransom for his help with the GBT observations. Support for this work was provided by NASA through the Spitzer Space Telescope Fellowship Program, under an award from Caltech. M.A.A. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-0602099. The Robert C. Byrd Green Bank Telescope is operated by the National Radio Astronomy Observatory, which is a facility of the US National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 27 TC 18 Z9 18 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2010 VL 721 IS 2 BP L158 EP L162 DI 10.1088/2041-8205/721/2/L158 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TB UT WOS:000282192200018 ER PT J AU Sanchez-Monge, A Palau, A Estalella, R Kurtz, S Zhang, QZ Di Francesco, J Shepherd, D AF Sanchez-Monge, Alvaro Palau, Aina Estalella, Robert Kurtz, Stan Zhang, Qizhou Di Francesco, James Shepherd, Debra TI IRAS 22198+6336: DISCOVERY OF AN INTERMEDIATE-MASS HOT CORE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: individual objects (IRAS 22198+6336); ISM: lines and bands; radio continuum: ISM; stars: formation ID STAR-FORMING REGIONS; BIPOLAR OUTFLOWS; JET HH-211; H2O MASERS; EMISSION; OBJECTS; PROTOSTARS; POPULATION; RESOLUTION; SAMPLE AB We present new Submillimeter Array and Plateau de Bure Interferometer observations of the intermediate-mass object IRAS 22198+6336 in the millimeter continuum and in several molecular line transitions. The millimeter continuum emission reveals a strong and compact source with a mass of similar to 5M(circle dot) and with properties of Class 0 objects. CO emission shows an outflow with a quadrupolar morphology centered on the position of the dust condensation. The CO outflow emission seems to come from two distinct outflows, one of them associated with SiO outflow emission. A large set of molecular lines has been detected toward a compact dense core clearly coincident with the compact millimeter source, and showing a velocity gradient perpendicular to the outflow traced by CO and SiO. The chemically rich spectrum and the rotational temperatures derived from CH(3)CN and CH(3)OH (100-150 K) indicate that IRAS 22198+6336 is harboring one of the few intermediate-mass hot cores known at present. C1 [Sanchez-Monge, Alvaro; Estalella, Robert] Univ Barcelona, Inst Ciencies Cosmos, Dept Astron & Meteorol, IEEC UB, E-08028 Barcelona, Spain. [Palau, Aina] Fac Ciencies, Inst Ciencies Espai, CSIC IEEC, E-08193 Barcelona, Spain. [Kurtz, Stan] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58090, Michoacan, Mexico. [Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Di Francesco, James] Herzberg Inst Astrophys, Conseil Natl Rech Canada, Victoria, BC, Canada. [Shepherd, Debra] Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Sanchez-Monge, A (reprint author), Univ Barcelona, Inst Ciencies Cosmos, Dept Astron & Meteorol, IEEC UB, Marti & Franques 1, E-08028 Barcelona, Spain. EM asanchez@am.ub.es OI Zhang, Qizhou/0000-0003-2384-6589 FU Spanish MICINN [AYA2008-06189-C03, ESP2007-65475-C02-02, Consolider-CSD2006-00070]; JAE-Doc CSIC; DGAPA-UNAM [IN101310]; European Social Fund FX We thank the anonymous referee for his/her useful comments. A.S-M. and A.P. are grateful to Esteban Araya for his help in analyzing the data, to Francesco Fontani and Asuncion Fuente for kindly providing complementary data, and also to Rob Gutermuth for his help with Spitzer data. A.S-M., A.P., and R.E. are supported by the Spanish MICINN grant AYA2008-06189-C03 (co-funded with FEDER funds). A.P. is supported by a JAE-Doc CSIC fellowship co-funded with the European Social Fund. This research has been partially funded by Spanish MICINN under the ESP2007-65475-C02-02 and Consolider-CSD2006-00070 grants. S.K. is partially supported by the DGAPA-UNAM grant IN101310. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 36 TC 17 Z9 17 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2010 VL 721 IS 2 BP L107 EP L111 DI 10.1088/2041-8205/721/2/L107 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TB UT WOS:000282192200007 ER PT J AU Wiersema, K Farrell, SA Webb, NA Servillat, M Maccarone, TJ Barret, D Godet, O AF Wiersema, K. Farrell, S. A. Webb, N. A. Servillat, M. Maccarone, T. J. Barret, D. Godet, O. TI A REDSHIFT FOR THE INTERMEDIATE-MASS BLACK HOLE CANDIDATE HLX-1: CONFIRMATION OF ITS ASSOCIATION WITH THE GALAXY ESO 243-49 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; X-rays: binaries; X-rays: individual (ESO 243-49 HLX-1) ID X-RAY SOURCES; XMM-NEWTON OBSERVATIONS; STATE AB In this Letter, we report a spectroscopic confirmation of the association of HLX-1, the brightest ultra-luminous X-ray (ULX) source, with the galaxy ESO 243-49. At the host galaxy distance of 95 Mpc, the maximum observed 0.2-10 keV luminosity is 1.2 x 10(42) erg s(-1). This luminosity is similar to 400 times above the Eddington limit for a 20 M(circle dot) black hole and has been interpreted as implying an accreting intermediate-mass black hole with a mass in excess of 500 M(circle dot) (assuming that the luminosity is a factor of 10 above the Eddington value). However, a number of other ULX sources have been later identified as background active galaxies or foreground sources. It has recently been claimed that HLX-1 could be a quiescent neutron star X-ray binary at a Galactic distance of only 2.5 kpc, so a definitive association with the host galaxy is crucial in order to confirm the nature of the object. Here, we report the detection of the Ha emission line for the recently identified optical counterpart at a redshift consistent with that of ESO 243-49. This finding definitively places HLX-1 inside ESO 243-49, confirming the extreme maximum luminosity and strengthening the case for it containing an accreting intermediate-mass black hole of more than 500 M(circle dot). C1 [Wiersema, K.; Farrell, S. A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Webb, N. A.; Barret, D.; Godet, O.] Univ Toulouse, UPS, CESR, F-31028 Toulouse 9, France. [Webb, N. A.; Barret, D.; Godet, O.] CNRS, UMR 5187, F-31028 Toulouse, France. [Servillat, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Maccarone, T. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. RP Wiersema, K (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England. FU National Science Foundation; STFC; European Union [215212]; [AR9-0013X]; [GO9-0102X] FX We thank M. C. Miller and the anonymous referees for their comments that helped to improve this Letter. We thank Tim de Zeeuw for granting us the VLT DDT observations. Based on observations made with ESO Telescopes at the Paranal Observatory under program ID 284.D-5008. IRAF is distributed by the National Optical Astronomy Observatories, which are operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation. S.A.F., K.W., and T.J.M. acknowledge STFC funding. T.J.M. thanks the European Union FP7 for support through grant 215212 Black Hole Universe. M.S. is supported in part by Chandra grants AR9-0013X and GO9-0102X. NR 19 TC 45 Z9 45 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2010 VL 721 IS 2 BP L102 EP L106 DI 10.1088/2041-8205/721/2/L102 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TB UT WOS:000282192200006 ER PT J AU Xu, X Narayanan, D Walker, C AF Xu, X. Narayanan, D. Walker, C. TI MOLECULAR DISK PROPERTIES IN EARLY-TYPE GALAXIES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: kinematics and dynamics; ISM: molecules ID PARTICLE HYDRODYNAMICS SIMULATIONS; CO-TO-H-2 CONVERSION FACTOR; ELLIPTIC GALAXIES; CO OBSERVATIONS; GALACTIC WINDS; STAR-FORMATION; BLACK-HOLES; H-I; GAS; MERGERS AB We study the simulated CO emission from elliptical galaxies formed in the mergers of gas-rich disk galaxies. The cold gas not consumed in the merger-driven starburst quickly resettles into a disk-like configuration. By analyzing a variety of arbitrary merger orbits that produce a range of fast-to slow-rotating remnants, we find that molecular disk formation is a fairly common consequence of gas-rich galaxy mergers. Hence, if a molecular disk is observed in an early-type merger remnant, it is likely the result of a "wet merger" rather than a "dry merger." We compare the physical properties from our simulated disks (e. g., size and mass) and find reasonably good agreement with recent observations. Finally, we discuss the detectability of these disks as an aid to future observations. C1 [Xu, X.; Walker, C.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Narayanan, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Xu, X (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. EM xxu@as.arizona.edu NR 50 TC 6 Z9 6 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2010 VL 721 IS 2 BP L112 EP L116 DI 10.1088/2041-8205/721/2/L112 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TB UT WOS:000282192200008 ER PT J AU Li, S Wang, DJ Gu, XD McShea, WJ AF Li, Sheng Wang, Dajun Gu, Xiaodong McShea, William J. TI Beyond pandas, the need for a standardized monitoring protocol for large mammals in Chinese nature reserves SO BIODIVERSITY AND CONSERVATION LA English DT Article DE Giant panda; Monitoring; Camera-trapping; Large mammals; China ID ESTIMATING SITE OCCUPANCY; PHOTOGRAPHIC RATES; ESTIMATE DENSITIES; CRYPTIC MAMMALS; CAMERA TRAPS; WILDLIFE; TIGERS; CONSERVATION; POPULATIONS; LANDSCAPE AB Monitoring programs are important for effective conservation and management programs. However, most of these programs rely on indirect sign surveys of elusive animals that often leave cryptic signs of their presence. In Sichuan Province, China, sign surveys are oriented mainly toward giant panda (Ailuropoda melanoleuca) populations but also are used to track other nationally listed species. We have developed and tested a monitoring system based on camera-trapping that can detect a wide range of large, terrestrial mammal and bird species within the reserves of Sichuan. This system is embedded within current protected area patrolling activities and relies on a partnership of management agencies, universities and international organizations. The international organizations and national universities primarily provide the training and assist with study design and data analysis. Data management and access is controlled at the regional level by the appropriate state agencies. Limitations to this system include the need for additional training and support to less developed reserves and the long-term availability of funds to support field staff. However, the potential return on investment is a consistent tracking of multiple species across diverse set of reserves, facilitating comparative analysis of results that will assist in adaptive management throughout the region. C1 [Li, Sheng; McShea, William J.] Smithsonian Conservat Biol Inst, Ctr Conservat Ecol, Front Royal, VA 22630 USA. [Li, Sheng; Wang, Dajun] Peking Univ, Coll Life Sci, Ctr Nat & Soc, Beijing 100871, Peoples R China. [Gu, Xiaodong] Sichuan Wildlife Conservat Management & Survey St, Sichuan Forestry Dept, Chengdu 610081, Peoples R China. RP Li, S (reprint author), Smithsonian Conservat Biol Inst, Ctr Conservat Ecol, 1500 Remount Rd, Front Royal, VA 22630 USA. EM lis@si.edu FU Smithsonian's National Zoological Park; Friends of the National Zoo; Peking University; Sichuan Forestry Department; China Wildlife Conservation Association; World Wildlife Fund China FX This project was supported by Smithsonian's National Zoological Park, Friends of the National Zoo, Peking University, Sichuan Forestry Department, China Wildlife Conservation Association, and World Wildlife Fund China. We thank Tangjiahe NR and Wolong NR for hosting the training courses and workshops, and all the reserve staffs that assisted with program management, data collection and logistic support. We also thank George B. Schaller and Colby Loucks for reviewing our manuscript and providing valuable comments. We had fruitful discussions with Lu Zhi, Wang Hongjia, Gu Haijun and Dai Bo on this project and the manuscript. NR 45 TC 9 Z9 22 U1 5 U2 35 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3115 J9 BIODIVERS CONSERV JI Biodivers. Conserv. PD OCT PY 2010 VL 19 IS 11 BP 3195 EP 3206 DI 10.1007/s10531-010-9886-x PG 12 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 663GG UT WOS:000282870700011 ER PT J AU Boyer, AG James, HF Olson, SL Grand-Mackie, JA AF Boyer, Alison G. James, Helen F. Olson, Storrs L. Grand-Mackie, Jack A. TI Long-term ecological change in a conservation hotspot: the fossil avifauna of Me Aure Cave, New Caledonia SO BIODIVERSITY AND CONSERVATION LA English DT Article DE Birds; Deforestation; Extinction; Owl pellet; Pacific islands; Radiocarbon; Sclerophyll forest; Subfossil; Turnix ID CERVUS-TIMORENSIS-RUSSA; NATIVE SCLEROPHYLL FOREST; SPECIES RICHNESS; EXTINCTION; ISLANDS; AREAS; BP AB Through the continuing accumulation of fossil evidence, it is clear that first human arrival on islands around the world was linked to a rise in the extinction rate for vertebrates. Bones in human-era fossil sites can also reveal changes in the composition and structure of ecological communities due to human environmental impacts. New Caledonia is a large and biogeographically distinct island in the southwest Pacific and is considered a critical priority for biodiversity conservation. We examined fossil birds from the Me Aure Cave site (WMD007), located in lowland dry forest on the west coast of New Caledonia. Accumulation of bird skeletal material in the cave was primarily through deposition in barn owl (Tyto alba) pellets. The site recorded the island-wide extinction of two species and extirpation of at least two other species from the lowlands in the past 1200 years. Species richness of birds in the stratigraphic deposit was quite high, reflecting the catholic diet of barn owls on islands, and many species have continued to persist near the site despite loss and degradation of the dry forest. However, we found substantial turnover in relative abundance of species in the cave deposit, with edge and open country birds becoming more common through time. These changes may reflect the severe reduction of dry forest habitat during the colonial period. This work provides a temporal record of avifaunal and environmental change in the threatened dry forest habitat that should be particularly informative for ongoing conservation and restoration efforts. C1 [Boyer, Alison G.] Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06520 USA. [Boyer, Alison G.; James, Helen F.; Olson, Storrs L.] Smithsonian Inst, Natl Museum Nat Hist, Div Birds, MRC 116, Washington, DC 20013 USA. [Grand-Mackie, Jack A.] Univ Auckland, Sch Geog & Environm, Auckland 1, New Zealand. RP Boyer, AG (reprint author), Yale Univ, Dept Ecol & Evolutionary Biol, 165 Prospect St, New Haven, CT 06520 USA. EM alison.boyer@yale.edu OI Boyer, Alison/0000-0002-4252-9725 FU Smithsonian Institution; NMNH; National Science Foundation [DBI-0805669] FX We are grateful to F. Desmoulins and the Programme de Conservation des Forets Seches for providing bird survey data from the Deux Freres forest and to Mr. G. SantaCroce for access to the Me Aure Cave site. P. Maurizot and C. Sand provided valuable advice that enabled our fieldwork in New Caledonia. We thank A. Wiley for pretreatment of the barn owl bones for radiocarbon dating. We thank D. Steadman and curatorial staff at the Florida Museum of Natural History and the National Museum of Natural History (NMNH) for their assistance. Funding was provided by a Smithsonian Institution Postdoctoral Fellowship to AGB and a NMNH grant to HFJ and AGB. The project was also partially supported by a National Science Foundation Postdoctoral Research Fellowship in Biological Informatics (DBI-0805669) to AGB. NR 61 TC 7 Z9 7 U1 1 U2 16 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3115 J9 BIODIVERS CONSERV JI Biodivers. Conserv. PD OCT PY 2010 VL 19 IS 11 BP 3207 EP 3224 DI 10.1007/s10531-010-9887-9 PG 18 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 663GG UT WOS:000282870700012 ER PT J AU Baeza, JA Piantoni, C AF Baeza, J. A. Piantoni, C. TI Sexual System, Sex Ratio, and Group Living in the Shrimp Thor amboinensis (De Man): Relevance to Resource-Monopolization and Sex-Allocation Theories SO BIOLOGICAL BULLETIN LA English DT Article ID LYSMATA-WURDEMANNI CARIDEA; LIFE-HISTORY; HERMAPHRODITIC SHRIMP; MATING TACTICS; DECAPODA; ANEMONE; HIPPOLYTIDAE; EVOLUTION; ANIMALS; CRUSTACEANS AB The sexual system of the symbiotic shrimp Thor amboinensis is described, along with observations on sex ratio and host-use pattern of different populations. We used a comprehensive approach to elucidate the previously unknown sexual system of this shrimp. Dissections, scanning electron microscopy, size-frequency distribution analysis, and laboratory observations demonstrated that T amboinensis is a protandric hermaphrodite: shrimp first mature as males and change into females later in life. Thor amboinensis inhabited the large and structurally heterogeneous sea anemone Stichoclactyla helianthus in large groups (up to 11 individuals) more frequently than expected by chance alone. Groups exhibited no particularly complex social structure and showed male-biased sex ratios more frequently than expected by chance alone. The adult sex ratio was male-biased in the four separate populations studied, one of them being thousands of kilometers apart from the others. This study supports predictions central to theories of resource monopolization and sex allocation. Dissections demonstrated that unusually large males were parasitized by an undescribed species of isopod (family Entoniscidae). Infestation rates were similarly low in both sexes (approximate to 11%-12%). The available information suggests that T. amboinensis uses pure search promiscuity as a mating system. This hypothesis needs to be formally tested with mating behavior observations and field measurements on the movement pattern of both sexes of the species. Further detailed studies on the lifestyle and sexual system of all the species within this genus and the development of a molecular phylogeny are necessary to elucidate the evolutionary history of gender expression in the genus Thor. C1 [Baeza, J. A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Baeza, J. A.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Baeza, J. A.] Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Larrondo 1281, Coquimbo, Chile. [Piantoni, C.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Piantoni, C.] Univ Sao Paulo, Inst Biociencias, Dept Fisiol, BR-05508900 Sao Paulo, Brazil. RP Baeza, JA (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. EM baezaa@si.edu OI Piantoni, Carla/0000-0002-1201-0041; Baeza, Juan Antonio/0000-0002-2573-6773 FU Marine Science Network; Smithsonian Institution through the Johnson and Hunterdon Oceanographic Research Endowment; National Geographic Society; Smithsonian Marine Station; Smithsonian Tropical Research Institute (STRI, Panama) FX We thank Sherry Reed and Narrisa Bax for their help during tedious hours of diving under harsh conditions while sampling sea anemones. We are also grateful to Mike Carpenter for his patience and help with the scheduling of diving trips and experimental work at CBC. Special thanks to Klaus Ruetzler, Tuck Hines, and Valerie Paul for their continuous support and funding for traveling to Belize. Jeff Shields and CRUST-L members were most helpful with identification of the parasite. Logistical support from Diane and Mark Littler and Barrett Brooks at Carrie Bow Cay, and James D. Reimer, Yoshikatsu Nakano, Yoshihisa Fujita, Obushi Masami, and Takuma Fujii at Okinawa, is deeply appreciated. We greatly appreciate Scott Whittaker's help with the SEM work. This research was funded by a Marine Science Network Grant from the Smithsonian Institution through the Johnson and Hunterdon Oceanographic Research Endowment (to JAB and Candy Feller) and by a Committee for Research and Exploration Grant of the National Geographic Society. Support from the Smithsonian Marine Station (Fort Pierce, Florida) Fellowship and Smithsonian Tropical Research Institute (STRI, Panama) Marine Fellowship is appreciated. Dr. Raymond T. Bauer and two anonymous referees critically reviewed the English as well as the content and provided very helpful comments. This article is CCRE and SMSFP contribution numbers 887 and 831, respectively. NR 62 TC 17 Z9 21 U1 2 U2 9 PU MARINE BIOLOGICAL LABORATORY PI WOODS HOLE PA 7 MBL ST, WOODS HOLE, MA 02543 USA SN 0006-3185 EI 1939-8697 J9 BIOL BULL-US JI Biol. Bull. PD OCT PY 2010 VL 219 IS 2 BP 151 EP 165 PG 15 WC Biology; Marine & Freshwater Biology SC Life Sciences & Biomedicine - Other Topics; Marine & Freshwater Biology GA 672YU UT WOS:000283625000008 PM 20972260 ER PT J AU Malo, AF Martinez-Pastor, F Alaks, G Dubach, J Lacy, RC AF Malo, Aurelio F. Martinez-Pastor, Felipe Alaks, Glen Dubach, Jean Lacy, Robert C. TI Effects of Genetic Captive-Breeding Protocols on Sperm Quality and Fertility in the White-Footed Mouse SO BIOLOGY OF REPRODUCTION LA English DT Article DE conservation breeding; docility; genetic adaptation to captivity; inbreeding depression; mean kinship; Peromyscus leucopus; reproductive success; testosterone ID G-DORCAS-NEGLECTA; INBREEDING DEPRESSION; OSMOTIC TOLERANCE; FLUCTUATING ASYMMETRY; CONSERVATION PROGRAMS; NATURAL-POPULATIONS; MEMBRANE INTEGRITY; EJACULATE QUALITY; GAZELLA-CUVIERI; DOMESTIC CAT AB Mice (Peromyscus leucopus noveboracensis) from a captive-breeding program were used to test the effects of three genetic breeding protocols (minimizing mean kinship [MK], random breeding, and selection for docility [DOC]) and inbreeding levels on sperm traits and fertility. Earlier, in generation 8, one DOC replicate went extinct because of poor reproductive success. By generation 10, spermatozoa from DOC mice had more acrosome and midpiece abnormalities, which were shown to be strong determinants of fertility, as well as lower sperm production and resistance to osmotic stress. In addition, determinants of fertility, including male and female components, were assessed in a comprehensive manner. Results showed that the probability (P) of siring litters is determined by sperm number, sperm viability, and midpiece and acrosome abnormalities; that the P of siring one versus two litters is determined by tail abnormalities; and that the total number of offspring is influenced by female size and proportion of normal sperm, showing the relative importance of different sperm traits on fertility. On average, males with 20% normal sperm sired one pup per litter, and males with 70% normal sperm sired eight pups per litter. Interestingly, the proportion of normal sperm was affected by docility but not by relatively low inbreeding. However, inbreeding depression in sperm motility was detected. In the MK group, inbreeding depression not only affected sperm motility but also fertility: An increase in the coefficient of inbreeding (f) of 0.03 reduced sperm motility by 30% and translated into an offspring reduction of three pups in second litters. A genetic load of 48 fecundity equivalents was calculated. C1 [Malo, Aurelio F.] Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Malo, Aurelio F.; Martinez-Pastor, Felipe; Alaks, Glen; Dubach, Jean; Lacy, Robert C.] Chicago Zool Soc, Dept Conservat Sci, Brookfield, IL USA. [Malo, Aurelio F.] Univ London Imperial Coll Sci Technol & Med, Sect Ecol & Evolut, Ascot, Berks, England. [Martinez-Pastor, Felipe] Univ Leon, ITRA ULE, INDEGSAL, E-24071 Leon, Spain. [Martinez-Pastor, Felipe] UCLM CSIC JCCM, IREC, Natl Wildlife Res Inst, Biol Reprod Grp, Albacete, Spain. RP Malo, AF (reprint author), Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. EM a.malo@imperial.ac.uk RI Malo, Aurelio/D-3973-2011; Martinez-Pastor, Felipe/B-4277-2008 OI Malo, Aurelio/0000-0002-0846-2096; Martinez-Pastor, Felipe/0000-0003-2987-4302 FU IMLS [IC-03-02-0186-02]; Spanish Ministry of Education and Science [FU2005-0893]; European Union [PIEF-GA-2008-220322]; Spanish Ministry of Science and Innovation; University of Castilla-La Mancha FX Supported by the IMLS Conservation Project Support Grant IC-03-02-0186-02. A.F.M. was a recipient of an MEC/Fulbright fellowship from the Spanish Ministry of Education and Science (FU2005-0893) and a Marie Curie fellowship from the European Union (PIEF-GA-2008-220322). F.M.-P. was supported by the Juan de la Cierva and Ramon y Cajal programs from the Spanish Ministry of Science and Innovation and by a travel grant from the University of Castilla-La Mancha. NR 76 TC 11 Z9 11 U1 2 U2 31 PU SOC STUDY REPRODUCTION PI MADISON PA 1691 MONROE ST,SUITE # 3, MADISON, WI 53711-2021 USA SN 0006-3363 EI 1529-7268 J9 BIOL REPROD JI Biol. Reprod. PD OCT PY 2010 VL 83 IS 4 BP 540 EP 548 DI 10.1095/biolreprod.110.085316 PG 9 WC Reproductive Biology SC Reproductive Biology GA 654JI UT WOS:000282163900006 PM 20519695 ER PT J AU Pelican, KM Spindler, RE Pukazhenthi, BS Wildt, DE Ottinger, MA Howard, J AF Pelican, Katharine M. Spindler, Rebecca E. Pukazhenthi, Budhan S. Wildt, David E. Ottinger, Mary A. Howard, JoGayle TI Progestin Exposure Before Gonadotropin Stimulation Improves Embryo Development after In Vitro Fertilization in the Domestic Cat SO BIOLOGY OF REPRODUCTION LA English DT Article DE embryo; gonadotropin-releasing hormone; oocyte metabolism; ovary; progesterone ID SUBSEQUENT LUTEAL FUNCTION; TIGER PANTHERA-TIGRIS; INVITRO FERTILIZATION; ARTIFICIAL-INSEMINATION; CHORIONIC-GONADOTROPIN; FOLLICLE DEVELOPMENT; OVARIAN ACTIVITY; LUTEINIZING-HORMONE; SEXUAL-BEHAVIOR; GNRH ANTAGONIST AB This study investigated the influence of progestin priming and ovarian quiescence on response to exogenous gonadotropin stimulation in the cat. Because a subpopulation of cats routinely ovulated spontaneously, there also was the opportunity to examine the ovary's reaction to the added impact of endogenously secreted progestagen. Queens were given 1) equine chorionic gonadotropin (eCG) plus human chorionic gonadotropin (hCG) only (control; n = 9 cats), 2) GnRH antagonist (antide) injections followed by eCG and hCG (n = 9), and 3) a progestin implant (levonorgestrel) followed by eCG and hCG (n = 9). Laparoscopy was used to assess ovarian activity and aspirate follicular oocytes that were graded on the basis of morphology. In five cats per treatment, half of the high-quality oocytes were assessed for glucose, pyruvate, and lactate metabolism as well as nuclear maturation. Remaining oocytes were inseminated in vitro, cultured, and examined at 72 h after insemination for cleavage. In the remaining four cats per treatment, all oocytes were inseminated in vitro and assessed at 72, 120, and 168 h after insemination for embryo developmental stage. Cats pretreated with progestin had more follicles and produced more embryos per donor (including at the combined morula/blastocyst stage) than controls or females treated with GnRH antagonist (P < 0.05). There were no differences among groups (P > 0.05) in oocyte carbohydrate metabolism, nuclear maturation metrics, or fertilization success, although there was a tendency toward improvements in all three (P < 0.2) in progestin-treated females. Interestingly, cats that spontaneously ovulated within 60 days of treatment onset also produced more embryos per cat than induced-ovulation counterparts (P < 0.05). Results indicate that prior exposure to exogenous progestin (via implant) or endogenous progestagen (via spontaneous ovulation) improves ovarian responsiveness to gonadotropins in the cat through a mechanism that is independent of the induction of ovarian quiescence. C1 [Pelican, Katharine M.; Spindler, Rebecca E.; Pukazhenthi, Budhan S.; Wildt, David E.; Howard, JoGayle] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA USA. [Pelican, Katharine M.; Ottinger, Mary A.] Univ Maryland, Dept Anim & Avian Sci, College Pk, MD 20742 USA. RP Pelican, KM (reprint author), Univ Minnesota, Dept Vet Populat Med, 385F Anim Sci Vet Med Bldg,1365 Gortner Ave, St Paul, MN 55108 USA. EM pelicank@umn.edu FU Smithsonian Institution; National Institutes of Health [K01-RR017310-05, KO1-RR00135]; Friends of the National Zoo; University of Maryland FX Supported by the Smithsonian Institution's Scholarly Studies Program, the National Institutes of Health (K01-RR017310-05), Friends of the National Zoo, and a Graduate Fellowship awarded to K.M.P. by the University of Maryland. B.S.P. was supported by funds from the National Institutes of Health (KO1-RR00135). Research conducted in partial fulfillment of requirements for the Ph.D. for K.M.P. at the University of Maryland. NR 70 TC 9 Z9 9 U1 0 U2 5 PU SOC STUDY REPRODUCTION PI MADISON PA 1691 MONROE ST,SUITE # 3, MADISON, WI 53711-2021 USA SN 0006-3363 EI 1529-7268 J9 BIOL REPROD JI Biol. Reprod. PD OCT PY 2010 VL 83 IS 4 BP 558 EP 567 DI 10.1095/biolreprod.109.083360 PG 10 WC Reproductive Biology SC Reproductive Biology GA 654JI UT WOS:000282163900008 PM 20463355 ER PT J AU Fontoura, T Cazetta, E do Nascimento, W Catenacci, L De Vleeschouwer, K Raboy, B AF Fontoura, Talita Cazetta, Eliana do Nascimento, Wander Catenacci, Lilian De Vleeschouwer, Kristel Raboy, Becky TI Diurnal frugivores on the Bromeliaceae Aechmea depressa LB Sm. from Northeastern Brazil: the prominent role taken by a small forest primate SO BIOTA NEOTROPICA LA English DT Article DE Atlantic Rainforest; epiphyte; golden-headed-lion tamarin; Leontopithecus chlysomelas AB Little is lcnown about frugivory of epiphytes. We investigated diurnal frugivores consuming Aechmea depressa, an endemic species from Southern Bahia, Brazil, through 67 hours of observation on three fruiting individuals. Infructescences were visited for 2% of the time and only by golden-headed lion tamarins (GHLTs; Leontopithecus chrysomelas). Aechmea depressa invests on physical defense to retain fruits for prolonged periods, however, GIALTs used their small size and dexterity to remove rigid bracts and extract fruits from the infructescence. Prior studies indicate GHLTs disperseAechmea seeds. Given the low visitation rates and probability that few frugivores successfully manipulate A. depressa fruits, we suggest that GHLTs are extremely important to maintaining the populations of this bromeliad species. C1 [Fontoura, Talita; Cazetta, Eliana; do Nascimento, Wander] Univ Estadual Santa Cruz UESC, Dept Ciencias Biol, BR-45650000 Ilheus, BA, Brazil. [Catenacci, Lilian] Univ Estadual Santa Cruz UESC, Dept Ciencias Biol, Programa Posgrad Zool, BR-45650000 Ilheus, BA, Brazil. [Catenacci, Lilian; De Vleeschouwer, Kristel; Raboy, Becky] Inst Estudos Socio Ambientais Sul Bahia, BR-45653145 Ilheus, BA, Brazil. [De Vleeschouwer, Kristel] Royal Zool Soc Antwerp, Ctr Res & Conservat, B-2018 Antwerp, Belgium. [Raboy, Becky] Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. RP Fontoura, T (reprint author), Univ Estadual Santa Cruz UESC, Dept Ciencias Biol, Rod Ilheus Itabuna,Km 16, BR-45650000 Ilheus, BA, Brazil. EM talita_fontoura@uol.com.br RI Cazetta, Eliana/F-3296-2010 OI Cazetta, Eliana/0000-0002-2209-2554 FU Universidade Estadual de Santa Cruz (UESC) FX The Universidade Estadual de Santa Cruz (UESC) provided funding for this project with additional infrastructure support from Projeto Mico Ledo-da-Cara-Dourada. Talita Fontoura, Wander do Nascimento and Becky Raboy had permission to conduct field work under the IBAMA licenses N 178/2006, 12714-1 and with additional approval from the owners of Fazenda Cabana da Serra/Incon. We are grateful to field assistants Gilvan Gomes Mota and Romano dos Santos Souza for helping us locate the focal clusters of A. depressa under observation in this study. NR 32 TC 4 Z9 4 U1 1 U2 3 PU REVISTA BIOTA NEOTROPICA PI CAMPINAS PA AV. DR. ROMEU TORTIMA, 388 - BARAO GERALDO, CEP 13084-520, CAMPINAS, SP, BRAZIL SN 1676-0603 J9 BIOTA NEOTROP JI Biota Neotrop. PD OCT-DEC PY 2010 VL 10 IS 4 SI SI BP 351 EP 354 PG 4 WC Biodiversity Conservation SC Biodiversity & Conservation GA V28BD UT WOS:000208655400042 ER PT J AU Frick, MG Zardus, JD Lazo-Wasem, EA AF Frick, Michael G. Zardus, John D. Lazo-Wasem, Eric A. TI A New Coronuloid Barnacle Subfamily, Genus and Species from Cheloniid Sea Turtles SO BULLETIN OF THE PEABODY MUSEUM OF NATURAL HISTORY LA English DT Article DE Caretta caretta; Chelonia mydas; sea turtles; epibiont; barnacle; new genus and species; Coronuloidea ID EPIBIONTS AB During a survey of the commensal barnacles of nesting and foraging sea turtles from the coastal waters of Florida and Georgia, USA, an undescribed species of platylepadid coronuloid barnacle was encountered, embedded within the carapace and plastron regions of host turtles. This new genus and species is described herein as Calyptolepas bjorndalae gen. et sp. nov. and is compared with other members of the family Platylepadidae. While similar in some respects to members of currently recognized platylepadid subfamilies, particularly Cylindrolepas darwiniana Pilsbry (Cylindrolepadinae Ross and Frick) and Platylepas decorata Darwin (Platylepadidae Newman and Ross), this new species bears an amalgamation of characters from these two subfamilies that require it to be placed into a new subfamily, Calyptolepadinae subfam. nov., also described herein. C1 [Frick, Michael G.] Smithsonian Natl Zool Pk, Friends Natl Zoo, Washington, DC 20013 USA. [Zardus, John D.] The Citadel, Dept Biol, Charleston, SC 29404 USA. [Lazo-Wasem, Eric A.] Yale Univ, Peabody Museum Nat Hist, Div Invertebrate Zool, New Haven, CT 06520 USA. RP Frick, MG (reprint author), Smithsonian Natl Zool Pk, Friends Natl Zoo, POB 37012,MRC-5516, Washington, DC 20013 USA. EM caretta05@aol.com; zardusjl@citadel.edu; eric.lazo-wasem@yale.edu NR 22 TC 8 Z9 8 U1 2 U2 4 PU PEABODY MUSEUM NATURAL HISTORY-YALE UNIV PI NEW HAVEN PA 170 WHITNEY AVE, PO BOX 208118, NEW HAVEN, CT 06520-8118 USA SN 0079-032X EI 2162-4135 J9 B PEABODY MUS NAT HI JI Bull. Peabody Mus. Natl. Hist. PD OCT PY 2010 VL 51 IS 2 BP 169 EP 177 DI 10.3374/014.051.0203 PG 9 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 673CQ UT WOS:000283636600003 ER PT J AU Cole, DG AF Cole, Daniel G. TI Archaeology and Landscape in the Mongolian Altai: An Atlas SO CARTOGRAPHY AND GEOGRAPHIC INFORMATION SCIENCE LA English DT Book Review C1 [Cole, Daniel G.] Smithsonian Inst, Washington, DC 20560 USA. RP Cole, DG (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 6 PU CARTOGRAPHY & GEOGRAPHIC INFOR SOC PI GAITHERSBURG PA 6 MONTGOMERY VILLAGE AVE, STE 403, GAITHERSBURG, MD 20879 USA SN 1523-0406 J9 CARTOGR GEOGR INF SC JI Cartogr. Geogr. Inf. Sci. PD OCT PY 2010 VL 37 IS 4 BP 319 EP 320 DI 10.1559/152304010793454345 PG 2 WC Geography SC Geography GA 686CW UT WOS:000284675400005 ER PT J AU Edgar, RG Clark, MA Dale, K Mitchell, DA Ord, SM Wayth, RB Pfister, H Greenhill, LJ AF Edgar, R. G. Clark, M. A. Dale, K. Mitchell, D. A. Ord, S. M. Wayth, R. B. Pfister, H. Greenhill, L. J. TI Enabling a high throughput real time data pipeline for a large radio telescope array with GPUs SO COMPUTER PHYSICS COMMUNICATIONS LA English DT Article DE Radio telescopes and instrumentation; Heterodyne receivers; Mathematical procedures and computer techniques; Computer science and technology ID MURCHISON WIDEFIELD ARRAY AB The Murchison Widefield Array (MWA) is a next-generation radio telescope currently under construction in the remote Western Australia Outback. Raw data will be generated continuously at 5 GiBs(-1), grouped into 8 s cadences. This high throughput motivates the development of on-site, real time processing and reduction in preference to archiving, transport and off-line processing. Each batch of 8 s data must be completely reduced before the next batch arrives. Maintaining real time operation will require a sustained performance of around 2.5 TFLOPs(-1) (including convolutions, FFTs, interpolations and matrix multiplications). We describe a scalable heterogeneous computing pipeline implementation, exploiting both the high computing density and FLOP-per-Watt ratio of modern GPUs. The architecture is highly parallel within and across nodes, with all major processing elements performed by GPUs. Necessary scatter-gather operations along the pipeline are loosely synchronized between the nodes hosting the GPUs. The MWA will be a frontier scientific instrument and a pathfinder for planned peta- and exa-scale facilities. (c) 2010 Elsevier B.V. All rights reserved. C1 [Edgar, R. G.; Clark, M. A.] Initiat Innovat Comp, Cambridge, MA 02138 USA. [Clark, M. A.; Mitchell, D. A.; Ord, S. M.; Wayth, R. B.; Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dale, K.; Pfister, H.] Sch Engn & Appl Sci, Cambridge, MA 02138 USA. RP Edgar, RG (reprint author), Initiat Innovat Comp, 29 Oxford St, Cambridge, MA 02138 USA. EM rge21@seas.harvard.edu; mikec@seas.harvard.edu; dale@eecs.harvard.edu; dmitchell@cfa.harvard.edu; sord@cfa.harvard.edu; rwayth@cfa.harvard.edu; pfister@seas.harvard.edu; greenhill@cfa.harvard.edu RI Wayth, Randall/B-2444-2013; Ord, Stephen/C-6138-2013 OI Wayth, Randall/0000-0002-6995-4131; FU Smithsonian Astrophysical Observatory; National Science Foundation [AST-0457585, PHY-0835713]; NVIDIA via the Harvard CUDA Center of Excellence FX We would like to thank NVIDIA for support via the Harvard CUDA Center of Excellence. Funding support was provided in part by the Smithsonian Astrophysical Observatory. This work was supported in part by the National Science Foundation through grants AST-0457585 and PHY-0835713. NR 27 TC 3 Z9 3 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0010-4655 J9 COMPUT PHYS COMMUN JI Comput. Phys. Commun. PD OCT PY 2010 VL 181 IS 10 BP 1707 EP 1714 DI 10.1016/j.cpc.2010.06.019 PG 8 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 651RU UT WOS:000281945600007 ER PT J AU Gaillou, E Post, JE Bassim, ND Zaitsev, AM Rose, T Fries, MD Stroud, RM Steele, A Butler, JE AF Gaillou, E. Post, J. E. Bassim, N. D. Zaitsev, A. M. Rose, T. Fries, M. D. Stroud, R. M. Steele, A. Butler, J. E. TI Spectroscopic and microscopic characterizations of color lamellae in natural pink diamonds SO DIAMOND AND RELATED MATERIALS LA English DT Article DE Natural pink diamond; Graining; Deformation twin; Plastic deformation; 405.5 nm center ID PLASTIC-DEFORMATION; RAMAN-SPECTROSCOPY; OPTICAL-CENTERS; CVD DIAMOND; CRYSTALS; GROWTH; PHOTOLUMINESCENCE; TEMPERATURE; PRESSURE; STRESS AB Nineteen natural, untreated, type laAB pink diamonds from various localities were studied. They display microscopic (similar to 1 mu m thick) pink lamellae along {111} in an otherwise colorless diamond. This coloration concentrated in lamellae is commonly referred to as "graining". The diamonds were examined using high spatial resolution spectroscopic methods and transmission electron microscopy. TEM revealed that a pink lamella consists of a cluster of paired microtwins created under stress by plastic deformation. Raman line shift and broadening associated with the twinned pink lamellae indicate the presence of residual stress. Ultraviolet-visible absorption spectra from each of the samples showed a broad absorption band centered at similar to 550 nm, the source of the pink color. Cathodoluminescence spectra of the pink lamellae are different from those of the bulk, colorless diamond matrix. Within the lamellae only, the H3 center is observed along with a less intense N3 center. In some samples, instead of the N3 center a new center with a zero phonon line at 405.5 nm is observed. This previously unreported 405.5 nm center has phonon sidebands qualitatively identical to the N3 center, and may be an N3 center modified by a specific environment. These results suggest that lattice vacancies were created during twinning resulting from plastic deformation, and that impurity centers (such as those containing nitrogen) trap some of the diffusing vacancies. Since the pink lamellae are still under residual stress, new or modified defect centers are created, e.g. H3 and N3. The color center(s) responsible for the pink color (550 nm absorption) was not identified, but likely is only present in diamonds that experienced plastic deformation. Reported annealing of plastically deformed brown diamonds, which results in a residual pink color, suggests that the pink color is stable under these high pressure, high temperature conditions. The reported observations that annealing plastically deformed brown diamonds results in a residual pink color and that the pink color does not anneal out under similar high pressure, high temperature conditions, suggests that the deformation inducing pink color occurs inside the Earth's mantle, whereas brown coloration might be induced during a more recent event such as the ascent of the diamond to the surface in a kimberlitic/lamproitic eruption. Published by Elsevier BM. C1 [Gaillou, E.; Post, J. E.; Rose, T.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Gaillou, E.; Bassim, N. D.; Stroud, R. M.; Butler, J. E.] USN, Res Lab, Washington, DC 20375 USA. [Zaitsev, A. M.] CUNY Coll Staten Isl, Staten Isl, NY 10314 USA. [Fries, M. D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Steele, A.] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. RP Gaillou, E (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC 0119,Natl Hist Bldg W,Loading Dock 10th & Con, Washington, DC 20560 USA. EM gailloue@si.edu RI Butler, James/B-7965-2008; Gaillou, Eloise/D-1753-2009; Stroud, Rhonda/C-5503-2008 OI Butler, James/0000-0002-4794-7176; Gaillou, Eloise/0000-0002-7949-268X; Stroud, Rhonda/0000-0001-5242-8015 FU Apollo Diamond; JCK Industry Fund; Coralyn Whitney Endowment Fund (Smithsonian Institution) FX The authors wish to thank Alan Collins for constructive discussion of the some spectroscopic results, as well as Fischione and Yoosuff Piccard for assistance with the Nanomilling of the FIB sections. We gratefully acknowledge grants from Apollo Diamond, the JCK Industry Fund, and the Coralyn Whitney Endowment Fund (Smithsonian Institution). We also thank Dr. Benjamin Rondeau and the anonymous person who reviewed this paper, and who improved the quality of this manuscript. NR 60 TC 25 Z9 25 U1 2 U2 20 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0925-9635 J9 DIAM RELAT MATER JI Diam. Relat. Mat. PD OCT PY 2010 VL 19 IS 10 BP 1207 EP 1220 DI 10.1016/j.diamond.2010.06.015 PG 14 WC Materials Science, Multidisciplinary SC Materials Science GA 654XB UT WOS:000282203300014 ER PT J AU Kaspari, M Chang, C Weaver, J AF Kaspari, Michael Chang, Charlotte Weaver, Johanna TI Salted roads and sodium limitation in a northern forest ant community SO ECOLOGICAL ENTOMOLOGY LA English DT Article DE Biogeochemistry; foraging; pollution; landscape; nutrition; soil ID SIZE-GRAIN HYPOTHESIS; BODY-SIZE; FRESH-WATER; FOOD; TEMPERATURE; POPULATION AB 1. Road salt is a common, anthropogenic source of NaCl in many temperate ecosystems. Sodium is also an essential and potentially limiting element for inland animal populations. This suggests that Na limitation in inland ecosystems, and hence attraction to Na sources, should increase with distance from salted roads. 2. In a North Temperate forest, we tested the prediction that Na recruitment would increase, as soil [Na] decreased, with distance from a salted two-lane highway. We presented ants with three concentrations of NaCl and sucrose solution along four pairs of transects ca 1, 10, 100, and 1000 m from the road. 3. Consistent with the Na-limitation hypothesis, the ratio of NaCl to sucrose use increased with distance from the road from 1:13 vials at 1 m to 1:5 vials at 1 km. Genera characterised by high Na use did not accumulate farther from the road. For the common and widespread Tapinoma sessile (Say), a 10-fold increase in distance from the road resulted in ants doubling their use of NaCl relative to sucrose. 4. Road salt is a well-known pollutant, especially of freshwater ecosystems. However, by suppressing plants and potentially promoting consumers, road salt may have more complex effects on terrestrial ecosystems, especially those far inland from oceanic aerosols. C1 [Kaspari, Michael] Univ Oklahoma, Dept Zool, Norman, OK 73019 USA. [Kaspari, Michael] Smithsonian Trop Res Inst, Balboa, Panama. [Chang, Charlotte] Pomona Coll, Dept Biol, Claremont, CA 91711 USA. [Weaver, Johanna] Oberlin Coll, OCMR, Oberlin, OH 44074 USA. RP Kaspari, M (reprint author), Univ Oklahoma, Dept Zool, Norman, OK 73019 USA. EM mkaspari@ou.edu OI Kaspari, Michael/0000-0002-9717-5768 FU NSF; Bullard Fellowship FX An NSF Research Experience for Undergraduates grant (to Harvard Forest), and a Bullard Fellowship (to MK) funded this research. A. Ellison and A. Smith were instrumental in providing logistical support; S. Cover was a continual source of insight into the New England ant community. NR 34 TC 13 Z9 13 U1 9 U2 40 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0307-6946 J9 ECOL ENTOMOL JI Ecol. Entomol. PD OCT PY 2010 VL 35 IS 5 BP 543 EP 548 DI 10.1111/j.1365-2311.2010.01209.x PG 6 WC Entomology SC Entomology GA 647TJ UT WOS:000281641900001 ER PT J AU Smith, JAM Reitsma, LR Marra, PP AF Smith, Joseph A. M. Reitsma, Leonard R. Marra, Peter P. TI Moisture as a determinant of habitat quality for a nonbreeding Neotropical migratory songbird SO ECOLOGY LA English DT Article DE body condition; body mass; habitat quality; migratory birds; nonbreeding winter habitat; Northern Waterthrush; Roosevelt Roads Naval Station, Puerto Rico; Seiurus noveboracensis ID WINTER SITE FIDELITY; NON-BREEDING SEASON; VENEZUELAN MANGROVES; NEARCTIC MIGRANTS; SAMPLING BLOOD; BODY CONDITION; STABLE-CARBON; TASSELED CAP; DRY SEASON; BIRDS AB Identifying the determinants of habitat quality for a species is essential for understanding how populations are limited and regulated. Spatiotemporal variation in moisture and its influence on food availability may drive patterns of habitat occupancy and demographic outcomes. Nonbreeding migratory birds in the neotropics occupy a range of habitat types that vary with respect to moisture. Using carbon isotopes and a satellite-derived measure of habitat moisture, we identified a moisture gradient across home ranges of radio-tracked Northern Waterthrush (Seiurus noveboracensis). We used this gradient to classify habitat types and to examine whether habitat moisture correlates with overwinter mass change and spring departure schedules of Northern Waterthrush over the late-winter dry season in the tropics. The two independent indicators of moisture revealed similar gradients that were directly proportional to body mass change as the dry season progressed. Birds occupying drier habitats declined in body mass over the study period, while those occupying wetter habitats increased in body mass. Regardless of habitat, birds lost an average of 7.6% of their mass at night, and mass recovery during the day trended lower in dry compared with wet habitats. This suggests that daily incremental shortfalls in mass recovery can lead to considerable season-long declines in body mass. These patterns resulted in consequences for the premigratory period, with birds occupying drier habitats having a delayed rate of fat deposition compared with those in wet habitats. Taken together with the finding that males, which are significantly larger than females, are also in better condition than females regardless of habitat suggests that high-quality habitats may be limited and that there may be competition for them. The habitat-linked variation in performance we observed suggests that habitat limitation could impact individual and population-level processes both during and in subsequent periods of the annual cycle. The linkage between moisture and habitat quality for a migratory bird indicates that the availability of high-quality habitats is dynamic due to variation in precipitation among seasons and years. Understanding this link is critical for ascertaining the impact of future climate change, particularly in the Caribbean basin, where a much drier future is predicted. C1 [Smith, Joseph A. M.; Marra, Peter P.] Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. [Reitsma, Leonard R.] Plymouth State Univ, Dept Biol Sci, Plymouth, NH 03264 USA. RP Smith, JAM (reprint author), Nature Conservancy, Delaware Bayshores Off, 2350 Route 47, Delmont, NJ 08314 USA. EM Joseph_Smith@tnc.org FU DoD FX This research was supported by a grant from the DoD Legacy Resources Management Program. We thank Daniel Brown, Ram Papish, Ryan Peters, Mark Pollock, T. J. Robinson, Jared Woodcock, Alicia Byrd, Sara Campbell, Bill Deluca, Brian Gibbons, and Karin Roux for their excellent and dedicated work in the field. We thank Winston Martinez and Oscar Diaz for facilitating our work at Roosevelt Roads Naval Station and the U. S. Forest Service Sabana Field Station and its staff for providing lodging and laboratory space. Thanks to William Gould and Gary Potts for help with acquiring imagery. Lee Weight at the Smithsonian Museum Support Center provided laboratory space and indispensable guidance during analysis of blood samples. We thank two anonymous reviewers for their thoughtful comments on the manuscript. Finally we thank Jean Lodge and Joe Wunderle for all of the assistance and hospitality they extended during our stay in Puerto Rico. NR 66 TC 35 Z9 35 U1 3 U2 32 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD OCT PY 2010 VL 91 IS 10 BP 2874 EP 2882 DI 10.1890/09-2212.1 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 660PE UT WOS:000282654700007 PM 21058548 ER PT J AU Voigt, CC Sorgel, K Dechmann, DKN AF Voigt, Christian C. Soergel, Karin Dechmann, Dina K. N. TI Refueling while flying: Foraging bats combust food rapidly and directly to power flight SO ECOLOGY LA English DT Article DE Chiroptera; diet; energetics; flight metabolism; foraging; lesser bulldog bat; Neotropics; Noctilio albiventris; Smithsonian Tropical Research Institute, Gamboa, Panama; substrate ID STABLE CARBON ISOTOPES; NECTAR-FEEDING BATS; SUBSTRATE PATHWAYS; ENERGY-EXPENDITURE; HOVERING FLIGHT; EXHALED BREATH; MIXING MODELS; WIND-TUNNEL; BIRDS; FUEL AB Flying vertebrates, such as bats, face exceptionally high energy costs during active flapping flight. Once airborne, energy turnover may exceed basal metabolic rate by a factor of up to 15. Here, we asked whether fuel that powers flight originates from exogenous (dietary nutrients), endogenous sources (mostly body lipids or glycogen), or a combination of both. Since most insectivorous bats fly continuously over relatively long time periods during foraging, we assumed that slowly mobilized glycogen, although suitable for supporting brief sallying flights, is inadequate to power aerial insect-hunting of bats. We hypothesized that the insect-feeding Noctilio albiventris rapidly mobilizes and combusts nutrients from insects it has just eaten instead of utilizing endogenous lipids. We used the stable carbon isotope ratio in the bats' exhaled breath (delta(13)C(brth)) to assess the origin of metabolized substrates of resting and flying N. albiventris in two nutritional conditions: fasted and recently fed. The breath of fasted resting bats was depleted in (13)C in relation to their insect diet (delta(13)C(diet)), indicating the combustion of (13)C depleted body lipids. In contrast to this, delta(13)C(brth) of bats that had recently fed closely matched delta(13)C(diet) in both resting and flying bats, suggesting a quick mobilization of ingested nutrients for metabolism. In contrast to most non-volant mammals, bats have evolved the ability to fuel their high energy expenditure rates through the rapid combustion of exogenous nutrients, enabling them to conquer the nocturnal niche of aerial insectivory. C1 [Voigt, Christian C.; Soergel, Karin; Dechmann, Dina K. N.] Leibniz Inst Zoo & Wildlife Res, Evolutionary Ecol Res Grp, D-10315 Berlin, Germany. [Dechmann, Dina K. N.] Univ Konstanz, Dept Biol, D-78457 Constance, Germany. [Dechmann, Dina K. N.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Voigt, CC (reprint author), Leibniz Inst Zoo & Wildlife Res, Evolutionary Ecol Res Grp, Alfred Kowalke Str 17, D-10315 Berlin, Germany. EM voigt@izw-berlin.de FU Deutsche Forschungsgemeinschaft [Vo890/11] FX We thank Antje S. Kretzschmar, Silke L. Voitgt-Heucke, Megan Lupek, Shai Pilosoph, and Apanie Wood for help during fieldwork, and Egbert Leigh and two anonymous reviewers for comments on the manuscript. We acknowledge the generous support of the Smithsonian Tropical Research Institute (STRI) and the Panamanian authorities. The experiments were carried out under permits from the Autoridad National del Ambiente (ANAM) of Panama and STRI IUCAC protocols. This work was financed by a grant from the Deutsche Forschungsgemeinschaft to C. C. Voigt and D. K. N. Dechmann (Vo890/11). NR 56 TC 26 Z9 26 U1 4 U2 42 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD OCT PY 2010 VL 91 IS 10 BP 2908 EP 2917 DI 10.1890/09-2232.1 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 660PE UT WOS:000282654700010 PM 21058551 ER PT J AU Reef, R Ball, MC Feller, IC Lovelock, CE AF Reef, Ruth Ball, Marilyn C. Feller, Ilka C. Lovelock, Catherine E. TI Relationships among RNA : DNA ratio, growth and elemental stoichiometry in mangrove trees SO FUNCTIONAL ECOLOGY LA English DT Article DE C : N : P; ecostoichiometry; growth rate hypothesis; nutrients; plant; shoot elongation ID C-N-P; BIOLOGICAL STOICHIOMETRY; CERIOPS-TAGAL; NUTRITIONAL CONDITION; NUTRIENT DYNAMICS; RNA/DNA RATIOS; LIFE-HISTORY; ATLANTIC COD; ACID; FOREST AB P>1. Growth rate is a fundamental property of organisms. In trees, growth is indeterminate and varies in space and time depending on resource availability, genetic constraints, competition and stress from biotic and abiotic environmental factors. 2. The ratio between the abundance of RNA and DNA in the tissue has been used to indicate recent growth rates in many systems, but not for trees. We assessed the applicability of using RNA : DNA ratios for assessing intraspecific and interspecific differences in growth rates in two species of mangrove trees under field conditions. We manipulated growth by fertilizing mangrove trees over a period of 4 years and measured tree growth as increments in linear extension of tagged shoots. The C, N and P contents per unit biomass were measured to test the hypothesis that faster growing organisms require more P per unit biomass (the Growth Rate Hypothesis). 3. We found that interspecific differences in the RNA : DNA ratio clearly reflected the difference in shoot elongation rates between the species. Intraspecific differences in RNA : DNA were significantly correlated with growth rates only for Avicennia marina and not for Ceriops australis. C : N and C : P ratios were lower in trees with higher growth rates and exhibited a negative correlation with RNA : DNA ratios. 4. Our results indicate that RNA : DNA ratios can reliably predict interspecific differences in growth rates between the two mangrove species and that RNA : DNA ratios can be used as an indication of variation in growth rate for Avicennia marina. The interaction between C : N : P ratios, RNA : DNA ratios and growth rates supported the Growth Rate Hypothesis on an interspecific level, but not on an intraspecific level. C1 [Reef, Ruth; Lovelock, Catherine E.] Univ Queensland, Ctr Marine Studies, St Lucia, Qld 4072, Australia. [Reef, Ruth; Lovelock, Catherine E.] Univ Queensland, Sch Biol Sci, St Lucia, Qld 4072, Australia. [Ball, Marilyn C.] Australian Natl Univ, Res Sch Biol, Div Plant Sci, Canberra, ACT 0200, Australia. [Feller, Ilka C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Reef, R (reprint author), Univ Queensland, Ctr Marine Studies, St Lucia, Qld 4072, Australia. EM r.reef@uq.edu.au RI Ball, Marilyn/D-1180-2009; Lovelock, Catherine/G-7370-2012; OI Lovelock, Catherine/0000-0002-2219-6855; Feller, Ilka/0000-0002-6391-1608 FU Australian Research Council [DP0774491, DP0986170]; Smithsonian Marine Science Network FX We thank N. Stromsoe and A. Main for their help with sample analysis and V. Benion, A. Grinham, A. Chamberlain and B. Clegg for assistance with fieldwork. U. Motro helped with statistical analysis. We thank M. Motro and the anonymous reviewers for their useful comments on this manuscript. Australian Research Council Discovery Projects DP0774491 and DP0986170 and the Smithsonian Marine Science Network funded this work. NR 62 TC 20 Z9 25 U1 4 U2 27 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0269-8463 J9 FUNCT ECOL JI Funct. Ecol. PD OCT PY 2010 VL 24 IS 5 BP 1064 EP 1072 DI 10.1111/j.1365-2435.2010.01722.x PG 9 WC Ecology SC Environmental Sciences & Ecology GA 651AA UT WOS:000281895800014 ER PT J AU den Tex, RJ Maldonado, JE Thorington, R Leonard, JA AF den Tex, Robert-Jan Maldonado, Jesus E. Thorington, Richard Leonard, Jennifer A. TI Nuclear copies of mitochondrial genes: another problem for ancient DNA SO GENETICA LA English DT Article DE Numt; aDNA; Sundasciurus; Mitochondria; Universal primers ID PSEUDOGENES; GENOME; NUMTS; SYSTEMATICS; RODENTIA; HISTORY AB The application of ancient DNA techniques is subject to many problems caused primarily by low quality and by low quantity of DNA. For these reasons most studies employing ancient DNA rely on the characterization of mitochondrial DNA, which is present in many more copies per cell than nuclear DNA and hence more copies are likely to survive. We used universal and taxon specific mitochondrial primers to amplify DNA from museum specimens, and found many instances where the amplification of nuclear copies of the mitochondrial gene (numts) instead of the targeted mitochondrial fragment had occurred. Furthermore, the likelihood of amplifying numts increased dramatically when universal primers were utilized. Here we suggest that ancient DNA practitioners must consider the possibility that numts can be amplified at higher rates than previously thought. This is another complication for ancient DNA studies, but it also suggests that more extensive inclusion of nuclear markers in ancient DNA studies should be feasible. C1 [den Tex, Robert-Jan; Leonard, Jennifer A.] Uppsala Univ, Dept Evolutionary Biol, S-75236 Uppsala, Sweden. [Maldonado, Jesus E.; Thorington, Richard] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Maldonado, Jesus E.; Leonard, Jennifer A.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Leonard, Jennifer A.] CSIC, Estn Biol Donana, Seville 41092, Spain. RP Leonard, JA (reprint author), Uppsala Univ, Dept Evolutionary Biol, Norbyvagen 18D, S-75236 Uppsala, Sweden. EM JLeonard@ebd.csic.es RI CSIC, EBD Donana/C-4157-2011; Leonard, Jennifer/A-7894-2010 OI CSIC, EBD Donana/0000-0003-4318-6602; Leonard, Jennifer/0000-0003-0291-7819 FU Smithsonian Restricted Endowment Walcott Fund; Swedish Research Council FX Samples were kindly provided by the National Museum of Natural History 'Naturalis' (formerly Rijksmuseum van Natuurlijke Historie), Leiden, The Netherlands; the Natural History Museum, London; and the United States National Museum of Natural History, Smithsonian Institution. This project was funded by the Smithsonian Restricted Endowment Walcott Fund and the Swedish Research Council. Logistical support was provided by the Center for Conservation and Evolutionary Genetics, National Zoological Park, Smithsonian Institution, USA. NR 22 TC 20 Z9 22 U1 1 U2 12 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0016-6707 J9 GENETICA JI Genetica PD OCT PY 2010 VL 138 IS 9-10 BP 979 EP 984 DI 10.1007/s10709-010-9481-9 PG 6 WC Genetics & Heredity SC Genetics & Heredity GA 657SG UT WOS:000282432000007 PM 20700629 ER PT J AU Goto, K Fukuda, K Senda, A Saito, T Kimura, K Glander, KE Hinde, K Dittus, W Milligan, LA Power, ML Oftedal, OT Urashima, T AF Goto, Kohta Fukuda, Kenji Senda, Akitsugu Saito, Tadao Kimura, Kazumasa Glander, Kenneth E. Hinde, Katie Dittus, Wolfgang Milligan, Lauren A. Power, Michael L. Oftedal, Olav T. Urashima, Tadasu TI Chemical characterization of oligosaccharides in the milk of six species of New and Old world monkeys SO GLYCOCONJUGATE JOURNAL LA English DT Article DE Old world monkey; New world monkey; Milk oligosaccharide; Rhesus macaque; Toque macaque; Baboon; Capuchin; Mantled howler; Squirrel monkey; N-glycolylneuraminic acid ID BIFIDOBACTERIUM-BIFIDUM; MASS-SPECTROMETRY; DIVERGENCE TIMES; COLOSTRUM; CHROMATOGRAPHY; COMBINATION; CHIMPANZEE; PRIMATES; GORILLA AB Human and great ape milks contain a diverse array of milk oligosaccharides, but little is known about the milk oligosaccharides of other primates, and how they differ among taxa. Neutral and acidic oligosaccharides were isolated from the milk of three species of Old World or catarrhine monkeys (Cercopithecidae: rhesus macaque (Macaca mulatta), toque macaque (Macaca sinica) and Hamadryas baboon (Papio hamadryas)) and three of New World or platyrrhine monkeys (Cebidae: tufted capuchin (Cebus apella) and Bolivian squirrel monkey (Saimiri boliviensis); Atelidae: mantled howler (Alouatta palliata)). The milks of these species contained 6-8% total sugar, most of which was lactose: the estimated ratio of oligosaccharides to lactose in Old World monkeys (1:4 to 1:6) was greater than in New World monkeys (1:12 to 1:23). The chemical structures of the oligosaccharides were determined mainly by H-1-NMR spectroscopy. Oligosaccharides containing the type II unit (Gal(beta 1-4)GlcNAc) were found in the milk of the rhesus macaque, toque macaque, Hamadryas baboon and tufted capuchin, but oligosaccharides containing the type I unit (Gal(beta 1-3)GlcNAc), which have been found in human and many great ape milks, were absent from the milk of all species studied. Oligosaccharides containing Lewis x (Gal(beta 1-4)[Fuc(alpha 1-3)]GlcNAc) and 3-fucosyl lactose (3-FL, Gal(beta 1-4)[Fuc(alpha 1-3)]Glc) were found in the milk of the three cercopithecid monkey species, while 2-fucosyl lactose (5'-FL, Fuc(alpha 1-2)Gal(beta 1-4)Glc) was absent from all species studied. All of these milks contained acidic oligosaccharides that had N-acetylneuraminic acid as part of their structures, but did not contain oligosaccharides that had N-glycolylneuraminic acid, in contrast to the milk or colostrum of great apes which contain both types of acidic oligosaccharides. Two GalNAc-containing oligosaccharides, lactose 3'-O-sulfate and lacto-N-novopentaose I (Gal(beta 1-3)[Gal(beta 1-4)GlcNAc(beta 1-6)]Gal(beta 1-4)Glc) were found only in the milk of rhesus macaque, hamadryas baboon and tufted capuchin, respectively. Further research is needed to determine the extent to which the milk oligosaccharide patterns observed among these taxa represent wider phylogenetic trends among primates and how much variation occurs among individuals or species. C1 [Goto, Kohta; Fukuda, Kenji; Senda, Akitsugu; Urashima, Tadasu] Obihiro Univ Agr & Vet Med, Grad Sch Food Hyg, Obihiro, Hokkaido 0808555, Japan. [Saito, Tadao] Tohoku Univ, Grad Sch Agr, Sendai, Miyagi 980, Japan. [Kimura, Kazumasa] Yakult Cent Inst, Kunitachi, Tokyo, Japan. [Glander, Kenneth E.] Duke Univ, Dept Evolutionary Anthropol, Durham, NC USA. [Hinde, Katie] Univ Calif Davis, Calif Natl Primate Res Ctr, Brain Mind & Behav Unit, Davis, CA 95616 USA. [Dittus, Wolfgang] Inst Fundamental Studies, Smithsonian Primate Biol Program, Kandy, Sri Lanka. [Milligan, Lauren A.] Univ Calif Santa Cruz, Dept Anthropol, Santa Cruz, CA 95064 USA. [Dittus, Wolfgang; Power, Michael L.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Nutr Lab, Washington, DC USA. [Oftedal, Olav T.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Urashima, T (reprint author), Obihiro Univ Agr & Vet Med, Grad Sch Food Hyg, Obihiro, Hokkaido 0808555, Japan. EM urashima@obihiro.ac.jp OI Power, Michael/0000-0002-6120-3528; Hinde, Katie/0000-0002-0528-866X FU National Institutes of Health [RR019970, RR000169]; US National Science Foundation [BNS-9510894]; Earthwatch Institute, Boston, MA; LSB Leakey Foundation [1965]; National Center for Research Resources (NCRR) [P40 RR01254]; National Institutes of Health (NIH) FX We thank Michael Jakubasz and Regina Eisert for assistance in selecting and preparing samples at the Nutrition Laboratory of the Smithsonian National Zoological Park. Collection of rhesus macaque milk was supported in part by National Institutes of Health grants RR019970 to John Capitanio and RR000169 to the California National Primate Research Center. Toque macaque field research was supported by grants to W. Dittus from the US National Science Foundation (BNS-9510894) and the Earthwatch Institute, Boston, MA, and Sunil Gunathilake assisted with the collection of milk samples. Collection of capuchin milk was supported by a grant to LA Milligan from the LSB Leakey Foundation 1965. Squirrel monkey research was made possible by Grant Number P40 RR01254 from the National Center for Research Resources (NCRR), a component of the National Institutes of Health (NIH). Mantled howler research was supported by a grant to K. Glander from the Earthwatch Institute, Boston, MA and Kay Izard assisted with collection of milks. The contents of this paper are solely the responsibility of the authors and do not necessarily reflect the official views of the funding agencies. Samples obtained from primate research institutes were collected under Animal Care and Use authorizations of these organizations and/or the universities of the coauthors. NR 50 TC 20 Z9 21 U1 1 U2 11 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0282-0080 J9 GLYCOCONJUGATE J JI Glycoconjugate J. PD OCT PY 2010 VL 27 IS 7-9 BP 703 EP 715 DI 10.1007/s10719-010-9315-0 PG 13 WC Biochemistry & Molecular Biology SC Biochemistry & Molecular Biology GA 695HO UT WOS:000285361400007 PM 21127965 ER PT J AU Ousley, SD Jones, EB AF Ousley, Stephen D. Jones, Erica B. TI Craniometric Variation in the Aleutians: Integrating Morphological, Molecular, Spatial, and Temporal Data SO HUMAN BIOLOGY LA English DT Article DE CEPHALIC INDEX; CRANIAL INDEX; ALEUT PREHISTORY; ALEUTIAN ISLANDS; CRANIOMETRIC VARIATION; TYPOLOGY ID REPLACEMENT; ESKIMOS AB Several hypotheses have been put forward about the origins and evolution of the inhabitants of the Aleutian Islands. Both Hrdlicka [The Aleutian and Commander Islands and Their Inhabitants ( Philadelphia: Wistar Institute of Anatomy and Biology, 1945)] and Laughlin ["The Alaska gateway viewed from the Aleutian Islands," in Papers on the Physical Anthropology of the American Indian, W. S. Laughlin, ed. ( New York: Viking Fund, 1951), 98-126] analyzed cranial morphology and came to somewhat different conclusions using a typological approach and limited analytical methods. Subsequent investigations using morphological data have not significantly improved our understanding of Aleut prehistory. More recently, radiocarbon dating and mitochondrial DNA analyses have shed light on Aleut genetic variation and changes over time, but better morphological methods using multivariate statistical analysis have not yet been used. We analyzed craniometric data using multivariate procedures and found that Aleuts demonstrate significant changes in cranial morphology over time, and these changes correspond to Hrdlicka's observations but may not necessarily reflect in-migration. The morphological changes were concentrated in the very aspects of morphology that are easily observable and that Hrdlicka most often measured, namely, cranial length, breadth, and height, but they were obscured when craniometric variation as a whole was analyzed. Also, we found that the morphological changes over time were not related to the changes in haplogroup frequencies over time, suggesting that migration into the Aleutians did not play a significant role in producing the morphological changes. However, craniometric variability apparently increases over time, suggesting in-migration, localized selection, and/or greater environmental heterogeneity. Our results contradict Laughlin's observations but may be more in line with his hypothesis of in situ evolutionary changes absent gene flow. In addition to selection, gene flow, and gene drift, however, sociocultural changes must also be considered as a factor in why morphology changed over time. C1 [Ousley, Stephen D.] Mercyhurst Coll, Dept Anthropol Archaeol, Erie, PA 16546 USA. [Jones, Erica B.] Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. RP Ousley, SD (reprint author), Mercyhurst Coll, Dept Anthropol Archaeol, Erie, PA 16546 USA. NR 28 TC 4 Z9 4 U1 1 U2 8 PU WAYNE STATE UNIV PRESS PI DETROIT PA 4809 WOODWARD AVE, DETROIT, MI 48201-1309 USA SN 0018-7143 J9 HUM BIOL JI Hum. Biol. PD OCT-DEC PY 2010 VL 82 IS 5-6 SI SI BP 629 EP 651 PG 23 WC Anthropology; Biology; Genetics & Heredity SC Anthropology; Life Sciences & Biomedicine - Other Topics; Genetics & Heredity GA 734MW UT WOS:000288339200008 PM 21417887 ER PT J AU Ghent, RR Gupta, V Campbell, BA Ferguson, SA Brown, JCW Fergason, RL Carter, LM AF Ghent, Rebecca R. Gupta, V. Campbell, B. A. Ferguson, S. A. Brown, J. C. W. Fergason, R. L. Carter, L. M. TI Generation and emplacement of fine-grained ejecta in planetary impacts SO ICARUS LA English DT Article DE Moon; Mars; Venus; Cratering; Radar observations ID CRATER EJECTA; VENUS; MOON; MAGELLAN; DEPOSITS; BASIN AB We report here on a survey of distal fine-grained ejecta deposits on the Moon, Mars, and Venus. On all three planets, fine-grained ejecta form circular haloes that extend beyond the continuous ejects and other types of distal deposits such as run-out lobes or ramparts. Using Earth-based radar images, we find that lunar fine-grained ejecta haloes represent meters-thick deposits with abrupt margins, and are depleted in rocks >= 1 cm in diameter. Martian haloes show low nighttime thermal IR temperatures and thermal inertia, indicating the presence of fine particles estimated to range from similar to 10 mu m to 10 mm. Using the large sample sizes afforded by global datasets for Venus and Mars, and a complete nearside radar map for the Moon, we establish statistically robust scaling relationships between crater radius R and fine-grained ejects run-out r* for all three planets. On the Moon, r* similar to R(-0.18) for craters 5-640 km in diameter. For Venus, radar-dark haloes are larger than those on the Moon, but scale as r* similar to R(-0.49), consistent with ejecta entrainment in Venus' dense atmosphere. On Mars, fine-ejecta haloes are larger than lunar haloes for a given crater size, indicating entrainment of ejects by the atmosphere or vaporized subsurface volatiles, but scale as R(-0.13), similar to the ballistic lunar scaling. Ejecta suspension in vortices generated by passage of the ejecta curtain is predicted to result in ejecta run-out that scales with crater size as R(1/2), and the wind speeds so generated may be insufficient to transport particles at the larger end of the calculated range. The observed scaling and morphology of the low-temperature haloes leads us rather to favor winds generated by early-stage vapor plume expansion as the emplacement mechanism for low-temperature halo materials. (C) 2010 Elsevier Inc. All rights reserved. C1 [Ghent, Rebecca R.; Gupta, V.; Ferguson, S. A.; Brown, J. C. W.] Univ Toronto, Dept Geol, Toronto, ON M5S 3B1, Canada. [Campbell, B. A.; Carter, L. M.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Fergason, R. L.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. RP Ghent, RR (reprint author), Univ Toronto, Dept Geol, 22 Russell St, Toronto, ON M5S 3B1, Canada. EM ghentr@geology.utoronto.ca RI Carter, Lynn/D-2937-2012 FU Natural Sciences and Engineering Research Council of Canada; NASA; PGG FX We thank Nadine Barlow and Goro Komatsu for constructive reviews, which greatly improved the quality of this paper. Taronish Pithawala and John Koziar assisted with halo identification. This work was supported by a grant from the Natural Sciences and Engineering Research Council of Canada to R.R.G., and by the NASA Planetary Astronomy and PGG Programs. Arecibo Observatory is part of the National Astronomy and Ionosphere Center, operated by Cornell University under a cooperative agreement with the NSF. The Green Bank Telescope is part of the National Radio Astronomy Observatory, an NSF facility operated under cooperative agreement by Associated Universities, Inc. NR 37 TC 17 Z9 17 U1 1 U2 8 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD OCT PY 2010 VL 209 IS 2 BP 818 EP 835 DI 10.1016/j.icarus.2010.05.005 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654VL UT WOS:000282199000047 ER PT J AU Judkins, HL Vecchione, M Roper, CFE Torres, J AF Judkins, Heather L. Vecchione, Michael Roper, Clyde F. E. Torres, Joseph TI Cephalopod species richness in the wider Caribbean region SO ICES JOURNAL OF MARINE SCIENCE LA English DT Article; Proceedings Paper CT Symposium of the Cephalopod-International-Advisory-Council CY SEP, 2009 CL Spanish Natl Res Council, Vigo, SPAIN SP Cephalopod Int Advisory Council HO Spanish Natl Res Council DE cephalopod distribution; species richness; wider Caribbean region ID LATITUDINAL DIVERSITY GRADIENTS; ATLANTIC-OCEAN; DEEP-SEA; MARINE MOLLUSKS; RAPOPORTS RULE; NORTH-ATLANTIC; PATTERNS; NEMATODES; RANGE; SIZE AB The cephalopods of the wider Caribbean region (western central Atlantic) were examined in terms of distribution and ecological importance. In all, 4190 preserved cephalopod specimens were identified and catalogued to produce regional maps of cephalopod distribution within the wider Caribbean. Regional species richness was examined with respect to Rapoport's rule (RR) and to determine possible cephalopod hotspots in the region. Rarefaction curves were used to normalize the samples of various size collected throughout the wider Caribbean. Cephalopods of the wider Caribbean within latitudinal bands from 8 to 308N do not support RR because they exhibit increasing species richness with increasing latitude. Eight subareas were chosen to compare species richness. Regionally, species richness appears to be patchy, with cephalopods concentrated more off the eastern Florida coast. There is a need for increased sampling throughout the wider Caribbean. Areas were lacking in samples, especially the central and southeastern parts of the region. There is a need to explore the systematics, life histories, and distribution patterns for this group of organisms in future. C1 [Judkins, Heather L.; Torres, Joseph] Univ S Florida, Coll Marine Sci, St Petersburg, FL 33701 USA. [Vecchione, Michael] Smithsonian Inst, Natl Museum Nat Hist, NMFS Natl Systemat Lab, Washington, DC 20013 USA. RP Judkins, HL (reprint author), Univ S Florida, Coll Marine Sci, St Petersburg, FL 33701 USA. EM judkins@mail.usf.edu NR 48 TC 0 Z9 0 U1 4 U2 15 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1054-3139 J9 ICES J MAR SCI JI ICES J. Mar. Sci. PD OCT PY 2010 VL 67 IS 7 BP 1392 EP 1400 DI 10.1093/icesjms/fsq092 PG 9 WC Fisheries; Marine & Freshwater Biology; Oceanography SC Fisheries; Marine & Freshwater Biology; Oceanography GA 648UH UT WOS:000281719300010 ER PT J AU McDonald, KA Grunbaum, D AF McDonald, Kathryn A. Gruenbaum, Daniel TI Swimming Performance in Early Development and the "Other" Consequences of Egg Size for Ciliated Planktonic Larvae SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article; Proceedings Paper CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2010 CL Seattle, WA SP Soc Integrat & Comparat Biol ID MARINE BENTHIC INVERTEBRATES; TO-ZYGOTIC TRANSITION; SEA-URCHIN EMBRYOS; CELL LINEAGE; REPRODUCTIVE STRATEGIES; CREPIDULA-FORNICATA; ECHINODERM LARVAE; NONFEEDING LARVAE; PATELLA-VULGATA; EVOLUTION AB The evolutionary significance of egg size in marine invertebrates is commonly perceived in energetic terms. Embryonic size should also have direct effects upon the forces that govern swimming, a behavior common to early larval development in the plankton. If swimming is ecologically important, early larvae may need to perform to a certain "standard", or threshold of speed and/or stability. The existence of performance standards in early development could therefore act to constrain the evolution of egg size and the evolution of development. Here we present the key parameters that characterize the upward swimming speed of ciliated spheroidal larvae moving at very low Reynolds numbers. The dependence of maximum supported mass upon larval size, and the independence of neutral-weight swimming speed from size, lead to hypotheses about scaling of swimming speed with size. Experimental studies with thirteen broadcast-spawning planktotrophs demonstrate that free-living embryonic swimmers in all of these species conform to a strong negative scaling of density with size that offsets increases in mass with increasing size. This trend suggests that swimming ability is broadly under selection in early development. In experimental studies and in a hydrodynamic model of larval swimming, the performance of trochophore larvae provides support for our hypothesized scaling relationships, and also for the concept of a standard in swimming speed. Echinoid blastulae, however, show relationships between speed and size that are not predicted by our scaling arguments. Results for echinoids suggest that differences in ciliary tip speed, or possibly in spatial density of cilia over the blastula's surface, result in significant differences in species' performance. Strong phyletic differences in the initial patterning and growth of structures used for swimming thus appear to cause significant differences in the relationship of swimming ability with embryo size. C1 [McDonald, Kathryn A.] Univ Washington, Friday Harbor Labs, Friday Harbor, WA 98250 USA. [McDonald, Kathryn A.] Smithsonian Trop Res Inst, DPO, AA 34002 USA. [Gruenbaum, Daniel] Univ Washington, Sch Oceanog, Seattle, WA 98195 USA. RP McDonald, KA (reprint author), Univ Washington, Friday Harbor Labs, Friday Harbor, WA 98250 USA. EM mcdonaldk2@si.edu FU National Science Foundation [OCE-0217304]; National Oceanic and Atmospheric Administration Washington [NA040AR170032]; Friday Harbor FX Friday Harbor-Achievement Rewards for College Scientists Fellowship (to K.A.M.); National Science Foundation support for K. A. M. came from grant (OCE-0217304 to R. R. S.); National Oceanic and Atmospheric Administration Washington Sea Grant (# NA040AR170032 to D.G.). NR 61 TC 10 Z9 10 U1 2 U2 14 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 EI 1557-7023 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD OCT PY 2010 VL 50 IS 4 BP 589 EP 605 DI 10.1093/icb/icq090 PG 17 WC Zoology SC Zoology GA 657TU UT WOS:000282437700010 PM 21558226 ER PT J AU Jud, NA Rothwell, GW Stockey, RA AF Jud, Nathan A. Rothwell, Gar W. Stockey, Ruth A. TI PALEOECOLOGICAL AND PHYLOGENETIC IMPLICATIONS OF SAXICAULIS MECKERTII GEN. ET SP. NOV.: A BENNETTITALEAN STEM FROM THE UPPER CRETACEOUS OF WESTERN NORTH AMERICA SO INTERNATIONAL JOURNAL OF PLANT SCIENCES LA English DT Article DE Bennettitales; borer; Cretaceous; oribatid mites; plant-animal interactions ID SEED-PLANT PHYLOGENY; CHIBA PREFECTURE; PETRIFIED PLANTS; ANGIOSPERMS; ORIGIN; TRUNK; CYCADEOIDEA; GNETALES; JAPAN; REEVALUATION AB A new anatomically preserved bennettitalean stem has been recovered from the Upper Cretaceous (Coniacian) Eden Main locality on Vancouver Island, British Columbia, Canada. The fossil, described as Saxicaulis meckertii gen. et sp. nov., is permineralized and consists of a eustelic stem with diverging non-girdling leaf traces, a narrow zone of dense wood, primary cortex, and adventitious roots. Important vegetative characters that differentiate bennettitalean stems from cycad stems are reviewed, and while the anatomy of the stem conforms to Bennettitales, it is not consistent with either the Williamsoniaceae or the Cycadeoidaceae as they are currently understood. This fossil documents greater structural diversity among Cretaceous bennettitaleans than previously known and tentatively documents an additional growth habit (underground stem). Co-occurring fossils and plant structure suggest this plant may have inhabited an environment prone to fires. Additionally, there is evidence for two forms of plant-animal interaction in the fossil. The first is a large gallery in the pith lined with wound reaction tissue and accessed through a 3-mm hole on the surface of the stem that represents a new type of herbivore damage for Bennettitales. Reaction tissue occurs in rings and plates throughout the plant body. Smaller galleries containing coprolites of oribatid mites and lacking wound reaction tissue are present in the cortex. The complexity of Upper Cretaceous bennettitalean plant-animal interactions through herbivory and detritivory is evaluated. C1 [Jud, Nathan A.] Smithsonian Inst, Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Jud, Nathan A.] Univ Maryland Coll Pk, Program Behav Ecol Evolut & Systemat, College Pk, MD 20742 USA. [Rothwell, Gar W.] Ohio Univ, Dept Environm & Plant Biol, Athens, OH 45701 USA. [Stockey, Ruth A.] Univ Alberta, Dept Biol Sci, Edmonton, AB T6G 2E9, Canada. RP Jud, NA (reprint author), Smithsonian Inst, Museum Nat Hist, Dept Paleobiol, POB 37012, Washington, DC 20560 USA. EM njud@umd.edu FU NSF [EF-0629819]; NSERC [A-6908] FX We are indebted to Dirk Meckert and Rick Ross on Vancouver Island and Steve Karafit, Hendrix College, for collecting assistance and to Steve Karafit for making the specimen available for detailed study. This work was supported in part by the NSF (grant EF-0629819 to G. W. Rothwell and R. A. Stockey) and the NSERC (grant A-6908 to R. A. Stockey). NR 85 TC 5 Z9 5 U1 2 U2 7 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1058-5893 J9 INT J PLANT SCI JI Int. J. Plant Sci. PD OCT PY 2010 VL 171 IS 8 BP 915 EP 925 DI 10.1086/655963 PG 11 WC Plant Sciences SC Plant Sciences GA 650UA UT WOS:000281876900010 ER PT J AU Lambert, AM Dudley, TL Saltonstall, K AF Lambert, Adam M. Dudley, Tom L. Saltonstall, Kristin TI Ecology and Impacts of the Large-Statured Invasive Grasses Arundo donax and Phragmites australis in North America SO INVASIVE PLANT SCIENCE AND MANAGEMENT LA English DT Article DE Biological invasions; ruderal; life form; functional group; invasive species ID GIANT REED; COMMON REED; BIOLOGICAL-CONTROL; SOUTHERN CALIFORNIA; TETRAMESA-ROMANA; TIDAL MARSHES; ALIEN PLANTS; REPRODUCTION; ARUNDINOIDEAE; EXPANSION AB Large-statured invasive grasses (LSIGs) constitute a distinct functional group with characteristic life history traits that facilitate colonization and aggressive growth in aquatic ecosystems, particularly those modified by human activities. These species typically form monocultures in the systems they invade and have wide-ranging and negative impacts on biodiversity and ecosystem processes. In March 2008, a special symposium was held as part of the Western Society of Weed Scientists annual meeting to synthesize our current knowledge of the ecological impacts and management of two notorious LSIGs: Arundo donax and Phragmites australis. In this volume of Invasive Plant Science and Management, symposium participants provide articles summarizing existing knowledge, recent research progress, and research needs for these two taxa. Here, we summarize the basic biology of these species and suggest the use of a more holistic approach to deal with the effects and management of LSIG invasions. C1 [Lambert, Adam M.] Univ Calif Santa Barbara, Inst Marine Sci, Santa Barbara, CA 93106 USA. Smithsonian Trop Res Inst, Panama City, Panama. RP Lambert, AM (reprint author), Univ Calif Santa Barbara, Inst Marine Sci, Santa Barbara, CA 93106 USA. EM lambert@msi.ucsb.edu NR 54 TC 21 Z9 21 U1 3 U2 56 PU WEED SCI SOC AMER PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044-8897 USA SN 1939-7291 EI 1939-747X J9 INVAS PLANT SCI MANA JI Invasive Plant Sci. Manag. PD OCT-DEC PY 2010 VL 3 IS 4 BP 489 EP 494 DI 10.1614/IPSM-D-10-00031.1 PG 6 WC Plant Sciences SC Plant Sciences GA 778MG UT WOS:000291707800014 ER PT J AU Saltonstall, K Lambert, A Meyerson, LA AF Saltonstall, Kristin Lambert, Adam Meyerson, Laura A. TI Genetics and Reproduction of Common (Phragmites australis) and Giant Reed (Arundo donax) SO INVASIVE PLANT SCIENCE AND MANAGEMENT LA English DT Article DE Clonal; hybridization; large-statured invasive grass; plant dispersal; rhizome ID TRIN EX STEUDEL; NORTH-AMERICA; SEEDLING GROWTH; SALT MARSHES; ASEXUAL REPRODUCTION; SEXUAL REPRODUCTION; CHROMOSOME-NUMBERS; CRYPTIC INVASION; UNITED-STATES; PLOIDY LEVEL AB Genetic diversity and reproductive characteristics may play an important role in the invasion process. Here, we review the genetic structure and reproductive characteristics of common reed and giant reed, two of the most aggressive, large-statured invasive grasses in North America. Common reed reproduces both sexually and asexually and has a complex population structure, characterized by three subspecies with overlapping distributions; of which, one is introduced, one native, and the third is of unknown origins. These three subspecies show varying levels of genetic diversity, with introduced common reed having high levels of nuclear diversity, indicating that multiple introductions have likely occurred. In contrast, giant reed has low genetic diversity and appears to reproduce solely via asexual fragments yet is highly aggressive in parts of its introduced range. Both species are well-adapted for growth in human-dominated landscapes, which is presumably facilitated by their rhizomatous growth habit. C1 [Saltonstall, Kristin] Smithsonian Trop Res Inst, Panama City, Panama. Eastern Connecticut State Univ, Dept Biol, Willimantic, CT 06226 USA. Univ Rhode Isl, Kingston, RI 02881 USA. RP Saltonstall, K (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama. EM kristin.saltonstall@aya.yale.edu RI Meyerson, Laura/K-9013-2012; Meyerson, Laura/D-4487-2013 FU Dr. Eldredge Bermingham; Eastern Connecticut State University; Center for Invasive Plant Management, Montana State University; U.S. Department of Agriculture Agricultural Experiment Station [0208537] FX We thank the organizers of the "Arundol Phragmites Symposium" at the Western Society of Weed Science annual meeting in 2008. We thank Tom Dudley for sharing his knowledge of Arundo donax ecology and reproduction and Jacques Brisson, Jane Molofsky, and two anonymous reviewers for their comments on earlier versions of the manuscript. K. S. thanks Dr. Eldredge Bermingham for financial support and use of his laboratory facilities at the Smithsonian Tropical Research Institute. A.M.L. received grant support from Eastern Connecticut State University and from the Center for Invasive Plant Management, Montana State University. L.A.M. received support from the U.S. Department of Agriculture Agricultural Experiment Station grant 0208537. NR 83 TC 28 Z9 28 U1 0 U2 43 PU WEED SCI SOC AMER PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044-8897 USA SN 1939-7291 J9 INVAS PLANT SCI MANA JI Invasive Plant Sci. Manag. PD OCT-DEC PY 2010 VL 3 IS 4 BP 495 EP 505 DI 10.1614/IPSM-09-053.1 PG 11 WC Plant Sciences SC Plant Sciences GA 778MG UT WOS:000291707800015 ER PT J AU Meyerson, LA Lambert, AM Saltonstall, K AF Meyerson, Laura A. Lambert, Adam M. Saltonstall, Kristin TI A Tale of Three Lineages: Expansion of Common Reed (Phragmites australis) in the U.S. Southwest and Gulf Coast SO INVASIVE PLANT SCIENCE AND MANAGEMENT LA English DT Article DE Hybridization; desert vegetation; food web; plant invasion; conservation ID NORTH-AMERICA; POPULATIONS; WETLANDS AB The common reed invasion in North America has spanned two centuries and is still ongoing. This expansion comprises two main forms: an introduced Eurasian lineage (identified here as "Introduced Phragmites") and a Gulf Coast lineage of unknown origin (identified here as "Gulf Coast Phragmites"). Both lineages are spreading beyond their current ranges and are colonizing Southwestern and Gulf Coast ecosystems where they have not previously existed. As a result, the native North American lineage of common reed (hereafter "native Phragmites") has declined in many places. The recent invasion of the U.S. Southwest by Introduced and Gulf Coast Phragmites lineages has made this the only region in the world colonized by all three lineages. Along the central Gulf Coast where Gulf Coast Phragmites remains the dominant form, Introduced Phragmites has also recently invaded the Mississippi River delta. The consequences of these new invasions are uncertain, but a rapid response is needed to protect native species and ecosystems and reduce future control costs. C1 [Meyerson, Laura A.] Univ Rhode Isl, Dept Nat Resources Sci, Kingston, RI 02881 USA. Univ Calif Santa Barbara, Inst Marine Sci, Santa Barbara, CA 93106 USA. Smithsonian Trop Res Inst, Panama City, Panama. RP Meyerson, LA (reprint author), Univ Rhode Isl, Dept Nat Resources Sci, 1 Greenhouse Rd, Kingston, RI 02881 USA. EM Laura_Meyerson@uri.edu RI Meyerson, Laura/K-9013-2012; Meyerson, Laura/D-4487-2013 NR 29 TC 22 Z9 23 U1 1 U2 31 PU WEED SCI SOC AMER PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044-8897 USA SN 1939-7291 J9 INVAS PLANT SCI MANA JI Invasive Plant Sci. Manag. PD OCT-DEC PY 2010 VL 3 IS 4 BP 515 EP 520 DI 10.1614/IPSM-D-09-00052.1 PG 6 WC Plant Sciences SC Plant Sciences GA 778MG UT WOS:000291707800017 ER PT J AU Borojevic, K Steiner, WE Gerisch, R Zazzaro, C Ward, C AF Borojevic, Ksenija Steiner, Warren E., Jr. Gerisch, Rainer Zazzaro, Chiara Ward, Cheryl TI Pests in an ancient Egyptian harbor SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Plants; Pests; Tenebrionidae; Shipworms; Red Sea; Egypt; Punt ID STORED PRODUCTS; PLANTS; RECORDS; INSECT AB Our investigations combine detailed identification and interpretation of plant remains and associated fauna and their mode of arrival in one of the rock-cut galleries, Cave 3, at the site of Mersa/Wadi Gawasis on Egypt's Red Sea coast. The site served as a staging area and harbor from which Middle Kingdom pharaohs launched seafaring expeditions to the land of Punt in the early second millennium BC. Quantities of wood, including ship timbers, fastenings, debris related to ship dismantling and reworking, and charcoal were excavated and analyzed. Evidence of marine mollusk infestation (shipworm) was abundant in Cave 3, as were the remains of insect pests of stored foods. We also report on a unique find of a plaster "spill" that preserved the floor of Cave 3 as it was when people worked in the gallery ca. 3800 years ago. The plaster spill created a sealed deposit of plant and insect remains with a diagnostic ceramic fragment, allowing us to securely associate insect remains and "hollow" spikelets of emmer wheat (Triticum dicoccum) recovered from the gallery. An impression of the beetle Trachyderma hispida and its associated exoskeleton fragments provide new evidence of this species as a potential pest not yet reported from an archaeological grain storage site in Egypt. The finding of Tenebroides mauritanicus from the same deposit is the earliest known association of this pest with stored grains. These unique finds shed new light on the risks associated with preserving food supplies, combating pest infestation, and dealing with marine organisms on land and at sea in the pharaonic harbor. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Borojevic, Ksenija] Boston Univ, Dept Archaeol, Boston, MA 02215 USA. [Steiner, Warren E., Jr.] Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. [Gerisch, Rainer] Free Univ Berlin, Inst Biol, D-14195 Berlin, Germany. [Zazzaro, Chiara] Univ Naples Orientale, Dipartemento Studi & Ric Africa & Paesi Arabi, Lab Archeol, I-80134 Naples, Italy. [Ward, Cheryl] Coastal Carolina Univ, Ctr Archaeol & Anthropol, Dept Hist, Conway, SC 29528 USA. RP Borojevic, K (reprint author), Boston Univ, Dept Archaeol, 675 Commonwealth Ave, Boston, MA 02215 USA. EM boro@bu.edu; steinerw@si.edu; Gerisch1@aol.com; c.zazzaro@exeter.ac.uk; cward@coastal.edu FU Ministry for the University and Research, Rome, Italy (FIRB); University of Naples "I'Orientale," Naples, Italy; Italian Institute for Africa; Orient, Rome, Italy; Glen Dash Charitable Foundation, Woodstock; SCIEM; University of Naples "Suor Orsola di Benincasa," Naples, Italy FX Funds for the archaeological expedition at Mersa/Wadi Gawasis were granted by the Ministry for the University and Research, Rome, Italy (FIRB 2003); University of Naples "I'Orientale," Naples, Italy; Italian Institute for Africa and the Orient, Rome, Italy; generous contributions by Mr. Wallace Sellers, Lahaska, PA; and the Glen Dash Charitable Foundation, Woodstock, CT. Prof. Otto Cichocki and Dr. Carla Pepe participated with Research funds from SCIEM 2000, Project 7, and the University of Naples "Suor Orsola di Benincasa," Naples, Italy, respectively. The first author (K.B.) thanks the following colleagues for their help with identification from the photos: Yoel Melamed and Mordai Kislev for the help of some of the ambiguous plant specimens, Rebecca Mountain for the help with the identification of the monocotyledons, and W. Van Neer for confirming the identification of ovicaprine coprolites. Paul Goldberg and Francesco Berna provided useful comments and Trina Arpin helped with editing. All five authors are grateful to Kathryn Bard and Rodolfo Fattovich for providing them with an opportunity to be part of the Mersa/Wadi Gawasis research team. NR 45 TC 3 Z9 3 U1 0 U2 11 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD OCT PY 2010 VL 37 IS 10 BP 2449 EP 2458 DI 10.1016/j.jas.2010.04.013 PG 10 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 643AX UT WOS:000281265900009 ER PT J AU del Hoyo-Melendez, JM Mecklenburg, MF AF del Hoyo-Melendez, Julio M. Mecklenburg, Marion F. TI A survey on the light-fastness properties of organic-based Alaska Native artifacts SO JOURNAL OF CULTURAL HERITAGE LA English DT Article DE Alaska Native artifacts; Light-fastness; Micro-fading tester; Ethnographic collections AB A series of light-fastness tests were conducted on a group of ethnographic objects that will be on exhibit at the Smithsonian Institution Arctic Studies Center, a recent addition to the Anchorage Museum at Rasmuson Center in Alaska. The objects surveyed belong to the collections of the Smithsonian National Museum of Natural History and the Smithsonian National Museum of the American Indian. This work was designed as a feasibility study on the use of a micro-fading tester as a non-contact and non-destructive technique to evaluate the light-stability of materials present in ethnographic collections. A broad range of objects containing a wide variety of materials were selected for the study. The materials investigated included a variety of dyes applied on silk, cotton, and wool substrates along with some unusual materials such as tanned skin and seal gut skin. The results from this investigation have allowed establishing exhibition recommendations taking into consideration the sensitivity of each object, light levels in the museum building, and estimated light exposures based on the duration of the exhibit. The micro-fading tester has proven to be a very useful tool for determining the light-stability of ethnographic materials without causing any harm to the objects. Objects containing equivalent materials are usually classified under a general category based on their probable sensitivity to light. However, micro-fading test results have permitted the detection of dissimilarities among some of these objects, which could be associated to variations in prior fading histories, the quality of raw materials, and different preparation methods. (C) 2010 Elsevier Masson SAS. All rights reserved. C1 [del Hoyo-Melendez, Julio M.; Mecklenburg, Marion F.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. RP del Hoyo-Melendez, JM (reprint author), Univ Politecn Valencia, Inst Univ Restaurac Patrimonio, Camino Vera S-N 14,Edificio 9B, Valencia 46022, Spain. EM judeho1@doctor.upv.es; mecklenburgm@si.edu RI del Hoyo-Melendez, Julio/B-1395-2012 OI del Hoyo-Melendez, Julio/0000-0003-2163-2149 FU Smithsonian Institution Office of Research and Training Services FX This research was supported through a Pre-Doctoral Fellowship from the Smithsonian Institution Office of Research and Training Services. The authors would like to thank the staff from the Anthropology Conservation Laboratory of the National Museum of the Natural History and also the staff from the Conservation Laboratory of the National Museum of the American Indian for authorizing the use of artifacts in their collections for this survey. Special thanks to Kim Cullen Cobb, Landis Smith and Michelle Austin-Dennehy for all their support and assistance in coordinating this project. The authors wish to express their gratitude to Magdalena Moskal for providing valuable comments to this work. NR 32 TC 6 Z9 6 U1 1 U2 7 PU ELSEVIER FRANCE-EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER PI PARIS PA 23 RUE LINOIS, 75724 PARIS, FRANCE SN 1296-2074 J9 J CULT HERIT JI J. Cult. Herit. PD OCT-DEC PY 2010 VL 11 IS 4 BP 493 EP 499 DI 10.1016/j.culher.2010.01.004 PG 7 WC Archaeology; Art; Chemistry, Analytical; Geosciences, Multidisciplinary; Materials Science, Multidisciplinary; Spectroscopy SC Archaeology; Art; Chemistry; Geology; Materials Science; Spectroscopy GA 660XO UT WOS:000282680500017 ER PT J AU Pruitt, RJ Culver, SJ Buzas, MA Corbett, DR Horton, BP Mallinson, DJ AF Pruitt, Rebecca J. Culver, Stephen J. Buzas, Martin A. Corbett, D. Reide Horton, Benjamin P. Mallinson, David J. TI MODERN FORAMINIFERAL DISTRIBUTION AND RECENT ENVIRONMENTAL CHANGE IN CORE SOUND, NORTH CAROLINA, USA SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article ID ALBEMARLE-ESTUARINE-SYSTEM; NEUSE RIVER ESTUARY; BENTHIC FORAMINIFERA; OUTER BANKS; PARALIC ENVIRONMENTS; MARSH FORAMINIFERA; CONTINENTAL-SHELF; CHESAPEAKE BAY; PAMLICO-SOUND; SEA-LEVEL AB Core Sound, a shallow, narrow estuarine lagoon located behind North Carolina's southern Outer Banks, was studied to document modern foraminiferal distributions and identify environmental changes during the past ca. 90 years. Seventy-six samples collected in 2004 were analyzed to establish the modern distribution and abundance of foraminifera. Cluster analysis defined four modern biofacies: Marsh (dominated by Trochammina inflata and Haplophragmoides wilberti), Estuarine High Salinity A (dominated by Ammonia parkinsoniana and Elphidium mexicanum), Estuarine High Salinity B (dominated by Ammonia parkinsoniana and Elphidium excavatum), and Estuarine Low Salinity (dominated by Ammotium salsum, Ammonia parkinsoniana and Elphidium gunteri). The four biofacies were also recognized by discriminant analysis. Comparison of the 2004 distributional data with those derived from samples collected in 1959 from central and eastern Core Sound revealed that Elphidium decreased while Ammonia increased in relative abundance. Other researchers have suggested that such a trend reflects increased eutrophication, although there is no independent evidence for this in Core Sound. The temporal comparison also showed that Quinqueloculina has become more widespread immediately adjacent to barrier islands, which might relate to an increase in subaquatic vegetation. Five short cores were taken in mainland bays on the western margin of Core Sound. Analysis of radionuclides ((210)Pb and (137)Cs) provided a chronostratigraphic framework for two of the cores. To aid paleoenvironmental interpretations, foraminiferal data from core sediments dated as ca. 90 yr were entered as unknowns into the modern distribution discriminant analysis. Samples from mainland bay cores were classified with modern biofacies and indicated no significant foraminiferal change in the mainland bays over the last ca. 90 years. C1 [Pruitt, Rebecca J.; Culver, Stephen J.; Corbett, D. Reide; Mallinson, David J.] E Carolina Univ, Dept Geol Sci, Greenville, NC 27858 USA. [Corbett, D. Reide] E Carolina Univ, Inst Coastal Sci & Policy, Greenville, NC 27858 USA. [Buzas, Martin A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Horton, Benjamin P.] Univ Penn, Dept Earth & Environm Sci, Philadelphia, PA 19104 USA. RP Pruitt, RJ (reprint author), E Carolina Univ, Dept Geol Sci, Greenville, NC 27858 USA. FU [02ERAG0044] FX We thank Jim Watson, John Woods, and Dorothea Ames for their technical assistance in the field and laboratory and Drs. P. Buzas-Stephens, E. Leorri, and B. Hayward for their reviews. This research is part of the North Carolina Coastal Geology Cooperative Program. Funding for the USGS cooperative agreement award 02ERAG0044 is gratefully acknowledged. NR 90 TC 11 Z9 11 U1 1 U2 15 PU CUSHMAN FOUNDATION FORAMINIFERAL RES PI CAMBRIDGE PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST, HARVARD UNIV, CAMBRIDGE, MA 02138 USA SN 0096-1191 J9 J FORAMIN RES JI J. Foraminifer. Res. PD OCT PY 2010 VL 40 IS 4 BP 344 EP 365 PG 22 WC Paleontology SC Paleontology GA 656RG UT WOS:000282353700004 ER PT J AU Chaimanee, V Warrit, N Chantawannakul, P AF Chaimanee, Veeranan Warrit, Natapot Chantawannakul, Panuwan TI Infections of Nosema ceranae in four different honeybee species SO JOURNAL OF INVERTEBRATE PATHOLOGY LA English DT Article DE Apis mellifera; Asian honeybee; Nosema ceranae; Nosema apis; Microsporidia ID APIS-MELLIFERA; MICROSPORIDIAN PARASITE; MOLECULAR CHARACTERIZATION; COLONY COLLAPSE; BEE; EUROPE AB The microsporidium Nosema ceranae is detected in honeybees in Thailand for the first time. This endoparasite has recently been reported to infect most Apis mellifera honeybee colonies in Europe, the US, and parts of Asia, and is suspected to have displaced the endemic endoparasite species, Nosema apis, from the western A. mellifera. We collected and identified species of microsporidia from the European honeybee (A. mellifera), the cavity nesting Asian honeybee (Apis cerana), the dwarf Asian honeybee (Apis florea) and the giant Asian honeybee (Apis dorsata) from colonies in Northern Thailand. We used multiplex PCR technique with two pairs of primers to differentiate N. ceranae from N. apis. From 80 A. mellifera samples, 62 (77.5%) were positively identified for the presence of the N. ceranae. Amongst 46 feral colonies of Asian honeybees (A. cerana, A. florea and A. dorsata) examined for Nosema infections, only N. ceranae could be detected. No N. apis was found in our samples. N. ceranae is found to be the only microsporidium infesting honeybees in Thailand. Moreover, we found the frequencies of N. ceranae infection in native bees to be less than that of A. mellifera. (C) 2010 Elsevier Inc. All rights reserved. C1 [Chaimanee, Veeranan; Chantawannakul, Panuwan] Chiang Mai Univ, Fac Sci, Dept Biol, Chiang Mai 50200, Thailand. [Warrit, Natapot] Chulalongkorn Univ, Fac Sci, Dept Biol, Ctr Excellence Entomol, Bangkok 10330, Thailand. [Warrit, Natapot] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Chantawannakul, P (reprint author), Chiang Mai Univ, Fac Sci, Dept Biol, Chiang Mai 50200, Thailand. EM panuwan@gmail.com FU Commission on Higher Education, Thailand; Thailand Research Fund [RSA 5280010] FX We would like to thank the Commission on Higher Education, Thailand for support by Grant funding under the program of Strategic Scholarships for Frontier Research Network for the Joint Ph.D. Program Thai Doctoral degree for this research. Also we acknowledge the Thailand Research Fund (RSA 5280010) for financial support. We are grateful to Dr. Yanping Chen, Dr. Ingemar Fries and Dr. Requel Martin-Hernandez for providing bee samples. NR 29 TC 25 Z9 25 U1 3 U2 14 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2011 J9 J INVERTEBR PATHOL JI J. Invertebr. Pathol. PD OCT PY 2010 VL 105 IS 2 BP 207 EP 210 DI 10.1016/j.jip.2010.06.005 PG 4 WC Zoology SC Zoology GA 650DN UT WOS:000281829300016 PM 20600087 ER PT J AU Pavicic, M McKay, BD Megill, ND Fresl, K AF Pavicic, Mladen McKay, Brendan D. Megill, Norman D. Fresl, Kresimir TI Graph approach to quantum systems SO JOURNAL OF MATHEMATICAL PHYSICS LA English DT Article ID KOCHEN-SPECKER THEOREM; SMALL STATE-SPACES; ORTHOMODULAR LATTICES; GREECHIE DIAGRAMS; HILBERT-SPACES; LOGIC; CONSTRUCTIONS; VARIETIES; MECHANICS; EQUATIONS AB Using a graph approach to quantum systems, we show that descriptions of 3-dim Kochen-Specker (KS) setups as well as descriptions of 3-dim spin systems by means of Greechie diagrams (a kind of lattice) that we find in the literature are wrong. Correct lattices generated by McKay-Megill-Pavicic (MMP) hypergraphs and Hilbert subspace equations are given. To enable future exhaustive generation of 3-dim KS setups by means of our recently found stripping technique, bipartite graph generation is used to provide us with lattices with equal numbers of elements and blocks (orthogonal triples of elements)-up to 41 of them. We obtain several new results on such lattices and hypergraphs, in particular, on properties such as superposition and orthoraguesian equations. (C) 2010 American Institute of Physics. [doi:10.1063/1.3491766] C1 [Pavicic, Mladen] Harvard Univ, Inst Theoret Atom Mol & Opt Phys, Dept Phys, Cambridge, MA 02138 USA. [Pavicic, Mladen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pavicic, Mladen] Univ Zagreb, Fac Civil Engn, Chair Phys, Zagreb 10000, Croatia. [McKay, Brendan D.] Australian Natl Univ, Sch Comp Sci, Canberra, ACT 0200, Australia. [Megill, Norman D.] Boston Informat Grp, Lexington, MA 02420 USA. [Fresl, Kresimir] Univ Zagreb, Fac Civil Engn, Dept Tech Mech, Zagreb 10000, Croatia. RP Pavicic, M (reprint author), Harvard Univ, Inst Theoret Atom Mol & Opt Phys, Dept Phys, Cambridge, MA 02138 USA. EM mpavicic@grad.hr FU U.S. National Science Foundation; Smithsonian Astrophysical Observatory and Ministry of Science, Education, and Sport of Croatia [082-0982562-3160] FX This work is supported by the U.S. National Science Foundation through a grant for the Institute for Theoretical Atomic, Molecular, and Optical Physics (ITAMP) at Harvard University and Smithsonian Astrophysical Observatory and Ministry of Science, Education, and Sport of Croatia through the Project No. 082-0982562-3160. NR 70 TC 6 Z9 6 U1 0 U2 3 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0022-2488 EI 1089-7658 J9 J MATH PHYS JI J. Math. Phys. PD OCT PY 2010 VL 51 IS 10 AR 102103 DI 10.1063/1.3491766 PG 31 WC Physics, Mathematical SC Physics GA 674MR UT WOS:000283750800003 ER PT J AU Lambert, JB Heckenbach, EA Wu, YY Santiago-Blay, JA AF Lambert, Joseph B. Heckenbach, Eric A. Wu, Yuyang Santiago-Blay, Jorge A. TI Characterization of Plant Exudates by Principal-Component and Cluster Analyses with Nuclear Magnetic Resonance Variables SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID GAS CHROMATOGRAPHY/MASS SPECTROMETRY; IONIZATION MASS-SPECTROMETRY; PATTERN-RECOGNITION; SPECTROSCOPY; NMR; CLASSIFICATION; SOLVENTS; RESINS; URINE AB Principal-component and cluster analyses have been applied to nuclear magnetic resonance data for exudates derived from both conifers and angiosperms in order to classify these materials on the basis of molecular structure. The method succeeds in distinguishing resins produced by the conifer families Araucariaceae, Cupressaceae, and Pinaceae from each other and from resins produced by the angiosperm family Fabaceae. Other exudate types, including gums, gum resins, and kinos, also are distinguished from each other and from the resins. C1 [Lambert, Joseph B.; Heckenbach, Eric A.; Wu, Yuyang] Northwestern Univ, Dept Chem, Evanston, IL 60208 USA. [Santiago-Blay, Jorge A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Lambert, JB (reprint author), Northwestern Univ, Dept Chem, 2145 Sheridan Rd, Evanston, IL 60208 USA. EM jlambert@northwestern.edu FU Gallaudet University FX The authors are grateful to grants from Gallaudet University for support of this work and to K. Moy for data reduction. Individuals who provided samples have been acknowledged previously.5.7-10 NR 22 TC 6 Z9 8 U1 0 U2 6 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0163-3864 EI 1520-6025 J9 J NAT PROD JI J. Nat. Prod. PD OCT PY 2010 VL 73 IS 10 BP 1643 EP 1648 DI 10.1021/np100318n PG 6 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA 668SB UT WOS:000283288900005 PM 20860390 ER PT J AU Rothman, LS Gordon, IE Barber, RJ Dothe, H Gamache, RR Goldman, A Perevalov, VI Tashkun, SA Tennyson, J AF Rothman, L. S. Gordon, I. E. Barber, R. J. Dothe, H. Gamache, R. R. Goldman, A. Perevalov, V. I. Tashkun, S. A. Tennyson, J. TI HITEMP, the high-temperature molecular spectroscopic database SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Spectroscopic database; Molecular spectroscopy; Molecular absorption; Line parameters; High-temperature spectroscopy; HITEMP ID POTENTIAL-ENERGY SURFACE; DIPOLE-MOMENT FUNCTION; EINSTEIN-A-COEFFICIENTS; BROADENED HALF-WIDTHS; WATER-VAPOR; LINE LIST; HITRAN DATABASE; CARBON-DIOXIDE; HIGH-ACCURACY; NITRIC-OXIDE AB A new molecular spectroscopic database for high-temperature modeling of the spectra of molecules in the gas phase is described. This database, called HITEMP, is analogous to the HITRAN database but encompasses many more bands and transitions than HITRAN for the absorbers H2O, CO2, CO, NO, and OH. HITEMP provides users with a powerful tool for a great many applications: astrophysics, planetary and stellar atmospheres, industrial processes, surveillance, non-local thermodynamic equilibrium problems, and investigating molecular interactions, to name a few. The sources and implementation of the spectroscopic parameters incorporated into HITEMP are discussed. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Rothman, L. S.; Gordon, I. E.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Barber, R. J.; Tennyson, J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Gamache, R. R.] Univ Massachusetts, Sch Marine Sci, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA. [Dothe, H.] Spectral Sci Inc, Burlington, MA 01803 USA. [Goldman, A.] Univ Denver, Dept Phys, Denver, CO 80208 USA. [Perevalov, V. I.; Tashkun, S. A.] Russian Acad Sci, Siberian Branch, Inst Atmospher Opt, Tomsk 634055, Russia. RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. EM LRothman@cfa.harvard.edu RI Tennyson, Jonathan/I-2222-2012; Tashkun, Sergey/E-8682-2014; OI Tennyson, Jonathan/0000-0002-4994-5238; Gordon, Iouli/0000-0003-4763-2841; Rothman, Laurence/0000-0002-3837-4847 FU NASA [NAG5-13534]; Planetary Atmospheres program [NNX10AB94G]; Spectral Sciences, Inc.; National Science Foundation [ATM-0803135]; Russian Fund of Basic Research [06-05-39016-(1)GammaPhiEH_a, 09-05-93105-HPiHalephJI_a] FX We acknowledge the support of NASA through the Earth Observing System (EOS) program under the Grant no. NAG5-13534 and the Planetary Atmospheres program under Grant no. NNX10AB94G. We also acknowledge the CHEMS (Computation of Highly Excited Molecular Spectra) SBIR project through Spectral Sciences, Inc. RRG acknowledges support of this research by the National Science Foundation through Grant no. ATM-0803135. VIP and SAT acknowledge support by the Russian Fund of Basic Research under the Grant nos. 06-05-39016-(1)Gamma Phi EH_a and 09-05-93105-H Pi H aleph JI_a. NR 85 TC 403 Z9 421 U1 6 U2 57 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD OCT PY 2010 VL 111 IS 15 SI SI BP 2139 EP 2150 DI 10.1016/j.jqsrt.2010.05.001 PG 12 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 643CE UT WOS:000281269800002 ER PT J AU Dubernet, ML Boudon, V Culhane, JL Dimitrijevic, MS Fazliev, AZ Joblin, C Kupka, F Leto, G Le Sidaner, P Loboda, PA Mason, HE Mason, NJ Mendoza, C Mulas, G Millar, TJ Nunez, LA Perevalov, VI Piskunov, N Ralchenko, Y Rixon, G Rothman, LS Roueff, E Ryabchikova, TA Ryabtsev, A Sahal-Brechot, S Schmitt, B Schlemmer, S Tennyson, J Tyuterev, VG Walton, NA Wakelam, V Zeippen, CJ AF Dubernet, M. L. Boudon, V. Culhane, J. L. Dimitrijevic, M. S. Fazliev, A. Z. Joblin, C. Kupka, F. Leto, G. Le Sidaner, P. Loboda, P. A. Mason, H. E. Mason, N. J. Mendoza, C. Mulas, G. Millar, T. J. Nunez, L. A. Perevalov, V. I. Piskunov, N. Ralchenko, Y. Rixon, G. Rothman, L. S. Roueff, E. Ryabchikova, T. A. Ryabtsev, A. Sahal-Brechot, S. Schmitt, B. Schlemmer, S. Tennyson, J. Tyuterev, V. G. Walton, N. A. Wakelam, V. Zeippen, C. J. TI Virtual atomic and molecular data centre SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Atomic data; Molecular data; Astrophysics; Atmospheric physics; Fusion; Radiation; Lighting; Space physics; Planetology ID SPECTROSCOPIC DATABASE; ONLINE DATABASE; ICE; ASTROCHEMISTRY; ATMOSPHERE; MIXTURES; PROFILE; BAND; CH4 AB The Virtual Atomic and Molecular Data Centre (VAMDC, http://www.vamdc.eu) is a European Union funded collaboration between groups involved in the generation, evaluation, and use of atomic and molecular data. VAMDC aims to build a secure, documented, flexible and interoperable e-science environment-based interface to existing atomic and molecular data. The project will cover establishing the core consortium, the development and deployment of the infrastructure and the development of interfaces to the existing atomic and molecular databases. It will also provide a forum for training potential users and dissemination of expertise worldwide. This review describes the scope of the VAMDC project; it provides a survey of the atomic and molecular data sets that will be included plus a discussion of how they will be integrated. Some applications of these data are also discussed. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Dubernet, M. L.] Univ Paris 06, CNRS INP, UMR 7092, Lab Phys Mol Atmosphere & Astrophys, F-75252 Paris 05, France. [Dubernet, M. L.; Roueff, E.] Observ Paris, CNRS INSU, UMR 8102, Lab Univers & Theories,Sect Meudon, F-92195 Meudon, France. [Boudon, V.] Univ Bourgogne, CNRS, UMR 5209, Lab Interdisciplinaire Carnot Bourgogne, F-21078 Dijon, France. [Culhane, J. L.] Univ Coll London, Mullard Space Sci Lab, Surrey RH5 6NT, England. [Dimitrijevic, M. S.] Astron Observ, Belgrade 11060, Serbia. [Fazliev, A. Z.; Perevalov, V. I.] Russian Acad Sci, Siberian Branch, VE Zuev Inst Atmospher Opt, Tomsk 634021, Russia. [Joblin, C.] Univ Toulouse 3, CNRS INSU, UMR 5187, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 9, France. [Kupka, F.] Univ Vienna, Fac Math, A-1090 Vienna, Austria. [Leto, G.] Osserv Astrofis Catania, Ist Nazl Astrofis, I-95123 Catania, Italy. [Le Sidaner, P.] Observ Paris, CNRS INSU, UMS 2201, VO Paris Data Ctr,Div Informat Observ, F-92195 Meudon, France. [Loboda, P. A.] All Russian Inst Tech Phys RFNTC VNIITF, Russian Fed Nucl Ctr, Snezhinsk 456770, Chelyabinsk Reg, Russia. [Mason, H. E.] Ctr Math Sci, Dept Appl Math & Theoret Phys, Cambridge CB3 0WA, England. [Mason, N. J.] Open Univ, Fac Sci, Milton Keynes MK7 6AA, Bucks, England. [Mendoza, C.; Nunez, L. A.] Univ Los Andes, CeCalCULA, Corp Parque Tecnol Merida, Ctr Nacl Calculo Cient, Merida 5101, Venezuela. [Mendoza, C.] Inst Venezolano Invest Cient, Ctr Fis, Caracas 1020A, Venezuela. [Nunez, L. A.] Univ Ind Santander, Esc Fis, GIRG, Bucaramanga, Colombia. [Mulas, G.] Osservatorio Astron Cagliari, Ist Nazl Astrofis, I-09012 Capoterra, CA, Italy. [Piskunov, N.] Uppsala Univ, Dept Phys & Astron, S-75120 Uppsala, Sweden. [Ralchenko, Y.] NIST, Atom Phys Div, Gaithersburg, MD 20899 USA. [Rothman, L. S.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Millar, T. J.] Queens Univ Belfast, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland. [Ryabchikova, T. A.] RAS, Inst Astron, Moscow 119017, Russia. [Ryabtsev, A.] RAS, Inst Spect, Troitsk 142190, Russia. [Sahal-Brechot, S.; Zeippen, C. J.] Observ Paris, CNRS INSU, UMR 8112, Lab Etud Rayonnement & Mat Astrophys, F-75014 Paris, France. [Schmitt, B.] Univ Grenoble 1, CNRS INSU, UMR 5109, Lab Planetol Grenoble, F-38041 Grenoble 9, France. [Schlemmer, S.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Tennyson, J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Tyuterev, V. G.] Univ Reims, UFR Sci Exactes & Nat, CNRS INP, Grp Spect Mol & Atmospher,UMR 6089, F-51687 Reims 2, France. [Rixon, G.; Walton, N. A.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Wakelam, V.] Univ Bordeaux, CNRS INSU, UMR 5804, Lab Astrophys Bordeaux, F-33271 Floirac, France. RP Dubernet, ML (reprint author), Univ Paris 06, CNRS INP, UMR 7092, Lab Phys Mol Atmosphere & Astrophys, Case 76,4 Pl Jussieu, F-75252 Paris 05, France. EM Marie-Lise.Dubernet-Tuckey@upmc.FR RI BOUDON, Vincent/A-4504-2010; Ralchenko, Yuri/B-7687-2011; Ralchenko, Yuri/E-9297-2016; Schmitt, Bernard/A-1064-2009; Tennyson, Jonathan/I-2222-2012; Mulas, Giacomo/B-7480-2013; Nunez, Luis/D-3404-2013; Schlemmer, Stephan/E-2903-2015; Leto, Giuseppe/N-3355-2015; OI Ralchenko, Yuri/0000-0003-0083-9554; Schmitt, Bernard/0000-0002-1230-6627; Tennyson, Jonathan/0000-0002-4994-5238; Mulas, Giacomo/0000-0003-0602-6669; Nunez, Luis/0000-0003-4575-5899; Wakelam, Valentine/0000-0001-9676-2605; Millar, Tom/0000-0001-5178-3656; Schlemmer, Stephan/0000-0002-1421-7281; Leto, Giuseppe/0000-0002-0040-5011; Rothman, Laurence/0000-0002-3837-4847 FU VAMDC [INFRA-2008-1.2.2, 239108] FX VAMDC is funded under the "Combination of Collaborative Projects and Coordination and Support Actions" Funding Scheme of The Seventh Framework Program. Call topic: INFRA-2008-1.2.2 Scientific Data Infrastructure. Grant Agreement number: 239108. NR 55 TC 104 Z9 109 U1 1 U2 18 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD OCT PY 2010 VL 111 IS 15 SI SI BP 2151 EP 2159 DI 10.1016/j.jqsa.2010.05.004 PG 9 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 643CE UT WOS:000281269800003 ER PT J AU Tennyson, J Bernath, PF Brown, LR Campargue, A Csaszar, AG Daumont, L Gamache, RR Hodges, JT Naumenko, OV Polyansky, OL Rothman, LS Toth, RA Vandaele, AC Zobov, NF Fally, S Fazliev, AZ Furtenbacher, T Gordon, IE Hu, SM Mikhailenko, SN Voronin, BA AF Tennyson, Jonathan Bernath, Peter F. Brown, Linda R. Campargue, Alain Csaszar, Attila G. Daumont, Ludovic Gamache, Robert R. Hodges, Joseph T. Naumenko, Olga V. Polyansky, Oleg L. Rothman, Laurence S. Toth, Robert A. Vandaele, Ann Carine Zobov, Nikolai F. Fally, Sophie Fazliev, Alexander Z. Furtenbacher, Tibor Gordon, Iouli E. Hu, Shui-Ming Mikhailenko, Semen N. Voronin, Boris A. TI IUPAC critical evaluation of the rotational-vibrational spectra of water vapor. Part II Energy levels and transition wavenumbers for (HDO)-O-16, (HDO)-O-17, and (HDO)-O-18 SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Water vapor; Transition wavenumbers; Atmospheric physics; Energy levels; MARVEL; Information system; Database; W@DIS; Infrared spectra; Microwave spectra; (HDO)-O-16; (HDO)-O-17; (HDO)-O-18 ID FOURIER-TRANSFORM SPECTROSCOPY; LASER-ABSORPTION SPECTROSCOPY; BEAM-MASER SPECTROSCOPY; HETERODYNE FREQUENCY MEASUREMENTS; LORENTZ-BROADENING COEFFICIENTS; LINE-SHIFT COEFFICIENTS; HIGH-RESOLUTION; CM(-1) REGION; MU-M; HYPERFINE STRUCTURE AB This is the second of a series of articles reporting critically evaluated rotational-vibrational line positions, transition intensities, pressure dependences, and energy levels, with associated critically reviewed assignments and uncertainties, for all the main isotopologues of water. This article presents energy levels and line positions of the following singly deuterated isotopologues of water: (HDO)-O-16, (HDO)-O-17, and (HDO)-O-18. The MARVEL (measured active rotational-vibrational energy levels) procedure is used to determine the levels, the lines, and their self-consistent uncertainties for the spectral regions 0-22708, 0-1674, and 0-12 105 cm(-1) for (HDO)-O-16, (HDO)-O-17, and (HDO)-O-18, respectively. For (HDO)-O-16, 54 740 transitions were analyzed from 76 sources, the lines come from spectra recorded both at room temperature and from hot samples. These lines correspond to 36 690 distinct assignments and 8818 energy levels. For (HDO)-O-17, only 485 transitions could be analyzed from three sources; the lines correspond to 162 MARVEL energy levels. For (HDO)-O-18, 8729 transitions were analyzed from 11 sources and these lines correspond to 1864 energy levels. The energy levels are checked against ones determined from accurate variational nuclear motion computations employing exact kinetic energy operators. This comparison shows that the measured transitions account for about 86% of the anticipated absorbance of (HDO)-O-16 at 296 K and that the transitions predicted by the MARVEL energy levels account for essentially all the remaining absorbance. The extensive list of MARVEL lines and levels obtained are given in the Supplementary Material of this article, as well as in a distributed information system applied to water, W@DIS, where they can easily be retrieved. In addition, the transition and energy level information for (H2O)-O-17 and (H2O)-O-18, given in the first paper of this series [Tennyson, et al. J Quant Spectr Rad Transfer 2009;110:573-96], has been updated. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Tennyson, Jonathan; Polyansky, Oleg L.] Univ London Univ Coll, Dept Phys & Astron, London WC1E 6BT, England. [Bernath, Peter F.] Univ York, York YO10 5DD, N Yorkshire, England. [Brown, Linda R.; Toth, Robert A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Campargue, Alain] Univ Grenoble 1, Grenoble, France. [Csaszar, Attila G.; Furtenbacher, Tibor] Eotvos Lorand Univ, Budapest, Hungary. [Daumont, Ludovic] Univ Reims, Reims, France. [Gamache, Robert R.] Univ Massachusetts, Lowell, MA USA. [Hodges, Joseph T.] NIST, Gaithersburg, MD 20899 USA. [Naumenko, Olga V.; Fazliev, Alexander Z.; Mikhailenko, Semen N.; Voronin, Boris A.] Russian Acad Sci, VE Zuev Inst Atmospher Opt, Tomsk 634021, Russia. [Polyansky, Oleg L.; Zobov, Nikolai F.] Russian Acad Sci, Inst Appl Phys, Nizhnii Novgorod, Russia. [Rothman, Laurence S.; Gordon, Iouli E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vandaele, Ann Carine] Inst Aeron Spatiale Belgique, B-1180 Brussels, Belgium. [Fally, Sophie] Univ Libre Bruxelles, Brussels, Belgium. [Hu, Shui-Ming] Univ Sci & Technol China, Lab Bond Select Chem, Hefei 230026, Peoples R China. RP Tennyson, J (reprint author), Univ London Univ Coll, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM j.tennyson@ucl.ac.UK RI Csaszar, Attila/A-5241-2009; Hu, Shuiming/C-4287-2008; Bernath, Peter/B-6567-2012; Tennyson, Jonathan/I-2222-2012; Voronin, Boris/A-3444-2014; OI Hu, Shuiming/0000-0002-1565-8468; Bernath, Peter/0000-0002-1255-396X; Tennyson, Jonathan/0000-0002-4994-5238; Voronin, Boris/0000-0002-8743-5554; Gordon, Iouli/0000-0003-4763-2841; Rothman, Laurence/0000-0002-3837-4847 FU International Union of Pure and Applied Chemistry [2004-035-1-100]; UK Natural Environment Research Council, the Royal Society [WWLC-008535-(reintegration) MCA FP6 EC]; Scientific Research Fund. of Hungary [OTKA K77825]; European Union; Russian Foundation for Basic Research; Belgian Federal Science Policy Office [EV/35/3A, SD/AT/01A, PRODEX 1514901NLSFe(IC)]; Communaute de Belgique (Action de Recherche Concertees); NASA [NNX08AD92G]; National Science Foundation [ATM-0803135]; CNRS (INSU) FX We all thank the International Union of Pure and Applied Chemistry for funding under project 2004-035-1-100 (A database of water transitions from experiment and theory). In addition, this work has received partial support from the UK Natural Environment Research Council, the Royal Society, Grant WWLC-008535-(reintegration) MCA FP6 EC, the Scientific Research Fund. of Hungary (Grant OTKA K77825), the European Union QUASAAR Marie Curie research training network, NATO, the Russian Foundation for Basic Research, the Belgian Federal Science Policy Office (contracts EV/35/3A, SD/AT/01A, PRODEX 1514901NLSFe(IC)), the Belgian National Fund for Scientific Research (FRFC contracts), the Communaute de Belgique (Action de Recherche Concertees), the NASA laboratory astrophysics program, NASA Earth Observing System (E0S), under Grant NNX08AD92G, the National Science Foundation, through Grant no. ATM-0803135, and the Programme National LEFE (CHAT) of CNRS (INSU). Part of the research described in this paper was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 150 TC 82 Z9 89 U1 8 U2 46 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD OCT PY 2010 VL 111 IS 15 SI SI BP 2160 EP 2184 DI 10.1016/j.jqsrt.2010.06.012 PG 25 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 643CE UT WOS:000281269800004 ER PT J AU Leshchishina, O Kassi, S Gordon, IE Rothman, LS Wang, L Campargue, A AF Leshchishina, Olga Kassi, Samir Gordon, Iouli E. Rothman, Laurence S. Wang, Le Campargue, Alain TI High sensitivity CRDS of the a(1)Delta X-g(3)Sigma(-)(g) band of oxygen near 1.27 mu m: Extended observations, quadrupole transitions, hot bands and minor isotopologues SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Oxygen; O-2; Electric quadrupole; Singlet delta; Cavity ring down spectroscopy ID CAVITY RINGDOWN SPECTROSCOPY; SUBMILLIMETER-WAVE SPECTRUM; MICROWAVE-ABSORPTION LINES; MOLECULAR-OXYGEN; GROUND-STATE; RAMAN-SPECTRUM; PRESSURE; O-16(2); O-2; COEFFICIENTS AB The CW-Cavity Ring Down Spectroscopy (CW-CRDS) technique has been used to record the high sensitivity absorption spectrum of the a(1)Delta(g)-X 3 Sigma(g)- band of oxygen near 1.27 mu m. The spectra were obtained between 7640 and 7917 cm(-1) with "natural" oxygen and with a sample highly enriched in 180. The absolute intensities of 376 and 643 oxygen transitions were measured in the two spectra. They include the alpha(1)Delta(g)-X (3)Sigma(-)(g) (0-0) bands of O-16(2), (OO)-O-16-O-18, (OO)-O-16-O-17, (OO)-O-17-O-18 and O-18(2). The (0-0) bands of O-16(2) and O-18(2) show weak quadrupole transitions with line intensities ranging from 1 x 10(-30) to 1.9 x 10(-28) cm/molecule. They are accompanied by the alpha(1)Delta(g)- X E-3; (1-1) hot bands, which are reported for the first time. The line profiles of the transitions of the (OO)-O-16-O-17 and (OO)-O-17-O-18 isotopologues were observed to be broadened due to an unresolved magnetic hyperfine structure. Accurate spectroscopic parameters of the different energy levels involved in the observed bands were derived from a global fit of the observed line positions, combined with microwave and Raman measurements available in the literature. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Leshchishina, Olga; Kassi, Samir; Wang, Le; Campargue, Alain] Univ Grenoble 1, CNRS, Spectrometrie Phys Lab, F-38402 St Martin Dheres, France. [Gordon, Iouli E.; Rothman, Laurence S.; Wang, Le] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Leshchishina, Olga] Zuev Inst Atmospher Opt, Lab Theoret Spect, Tomsk 634021, Russia. RP Campargue, A (reprint author), Univ Grenoble 1, CNRS, Spectrometrie Phys Lab, F-38402 St Martin Dheres, France. EM Alain.CAMPARGUE@ujf-grenoble.fr FU ANR [NT09_436466]; NASA [NAGS-13534] FX We are very thankful to Shanshan Yu for her help in using the SPF1T program. Part of this work was performed at Grenoble University under the ANR project "IDEO" (NT09_436466). The HITRAN database is supported by NASA through the Earth Observing System (EOS) program under the Grant NAGS-13534. NR 42 TC 24 Z9 24 U1 0 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD OCT PY 2010 VL 111 IS 15 SI SI BP 2236 EP 2245 DI 10.1016/j.jqsrt.2010.05.014 PG 10 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 643CE UT WOS:000281269800009 ER PT J AU Lamouroux, J Tran, H Laraia, AL Gamache, RR Rothman, LS Gordon, IE Hartmann, JM AF Lamouroux, J. Tran, H. Laraia, A. L. Gamache, R. R. Rothman, L. S. Gordon, I. E. Hartmann, J. -M. TI Updated database plus software for line-mixing in CO2 infrared spectra and their test using laboratory spectra in the 1.5-2.3 mu m region SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE CO2; Line mixing; Infrared spectra; Remote sensing ID MOLECULAR SPECTROSCOPIC DATABASE; ATMOSPHERIC CO2; WING REGIONS; Q BRANCHES; BANDS; MODEL; TEMPERATURE; COMPUTATION; ISOTOPOMERS; INTENSITIES AB In a previous series of papers, a model for the calculation of CO2-air absorption coefficients taking line-mixing into account and the corresponding database/software package were described and widely tested. In this study, we present an update of this package, based on the 2008 version of HITRAN, the latest currently available. The spectroscopic data for the seven most-abundant isotopologues are taken from HITRAN. When the HITRAN data are not complete up to J ''=70, the data files are augmented with spectroscopic parameters from the CD5D-296 database and the high-temperature CDSD-1000 if necessary. Previously missing spectroscopic parameters, the air-induced pressure shifts and CO2 line broadening coefficients with H2O, have been added. The quality of this new database is demonstrated by comparisons of calculated absorptions and measurements using CO2 high-pressure laboratory spectra in the 1.5-2.3 mu m region. The influence of the imperfections and inaccuracies of the spectroscopic parameters from the 2000 version of HITRAN is clearly shown as a big improvement of the residuals is observed by using the new database. The very good agreements between calculated and measured absorption coefficients confirm the necessity of the update presented here and further demonstrate the importance of line-mixing effects, especially for the high pressures investigated here. The application of the updated database/software package to atmospheric spectra should result in an increased accuracy in the retrieval of CO2 atmospheric amounts. This opens improved perspectives for the space-borne detection of carbon dioxide sources and sinks. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Lamouroux, J.; Laraia, A. L.; Gamache, R. R.] Univ Massachusetts, Sch Marine Sci, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA. [Tran, H.; Hartmann, J. -M.] Univ Paris 12, CNRS, UMR 7583, LISA, F-94010 Creteil, France. [Tran, H.; Hartmann, J. -M.] Univ Paris 07, CNRS, UMR 7583, LISA, F-94010 Creteil, France. [Rothman, L. S.; Gordon, I. E.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. RP Hartmann, JM (reprint author), Univ Massachusetts, Sch Marine Sci, Dept Environm Earth & Atmospher Sci, 1 Univ Ave, Lowell, MA 01854 USA. EM hartmann@lisa.univ-paris12.fr RI Tran, Ha/I-5076-2013 FU National Science Foundation [ATM-0803135]; Centre National d'Etudes Spatiales FX J. Lamouroux, A.L. Laraia, and R.R. Gamache are pleased to acknowledge support of this research by the National Science Foundation through Grant no. ATM-0803135. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Science Foundation. The authors from LISA acknowledge support by the TOSCA program of the Centre National d'Etudes Spatiales. NR 27 TC 54 Z9 59 U1 0 U2 23 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD OCT PY 2010 VL 111 IS 15 SI SI BP 2321 EP 2331 DI 10.1016/j.jqsrt.2010.03.006 PG 11 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 643CE UT WOS:000281269800018 ER PT J AU Hazari, Z Sonnert, G Sadler, PM Shanahan, MC AF Hazari, Zahra Sonnert, Gerhard Sadler, Philip M. Shanahan, Marie-Claire TI Connecting High School Physics Experiences, Outcome Expectations, Physics Identity, and Physics Career Choice: A Gender Study SO JOURNAL OF RESEARCH IN SCIENCE TEACHING LA English DT Article DE gender; females; physics education; identity; survey; career choice; pedagogy ID SELF-CONCEPT; COLLEGE-STUDENTS; EDUCATIONAL EXPECTATIONS; UNIVERSITY PHYSICS; SCIENCE CLASSROOMS; ACHIEVEMENT; GIRLS; PERFORMANCE; INTERESTS; MATH AB This study explores how students' physics identities are shaped by their experiences in high school physics classes and by their career outcome expectations. The theoretical framework focuses on physics identity and includes the dimensions of student performance, competence, recognition by others, and interest. Drawing data from the Persistence Research in Science and Engineering (PRiSE) project, which surveyed college English students nationally about their backgrounds, high school science experiences, and science attitudes, the study uses multiple regression to examine the responses of 3,829 students from 34 randomly selected US colleges/universities. Confirming the salience of the identity dimension for young persons' occupational plans, the measure for students' physics identity used in this study was found to strongly predict their intended choice of a physics career. Physics identity, in turn, was found to correlate positively with a desire for an intrinsically fulfilling career and negatively with a desire for personal/family time and opportunities to work with others. Physics identity was also positively predicted by several high school physics characteristics/experiences such as a focus on conceptual understanding, real-world/contextual connections, students answering questions or making comments, students teaching classmates, and having an encouraging teacher. Even though equally beneficial for both genders, females reported experiencing a conceptual focus and real-world/contextual connections less frequently. The explicit discussion of under-representation of women in science was positively related to physics identity for female students but had no impact for male students. Surprisingly, several experiences that were hypothesized to be important for females' physics identity were found to be non-significant including having female scientist guest speakers, discussion of women scientists' work, and the frequency of group work. This study exemplifies a useful theoretical framework based on identity, which can be employed to further examine persistence in science, and illustrates possible avenues for change in high school physics teaching. (C) 2010 Wiley Periodicals, Inc. J Res Sci Teach 47: 978-1003, 2010 C1 [Hazari, Zahra] Clemson Univ, Dept Engn & Sci Educ, Clemson, SC USA. [Hazari, Zahra] Clemson Univ, Dept Math Sci, Clemson, SC USA. [Sonnert, Gerhard; Sadler, Philip M.] Harvard Smithsonian Ctr Astrophys, Sci Educ Dept, Cambridge, MA 02138 USA. [Shanahan, Marie-Claire] Univ Alberta, Dept Elementary Educ, Edmonton, AB, Canada. RP Hazari, Z (reprint author), Clemson Univ, Dept Engn & Sci Educ, Clemson, SC USA. EM zahra@clemson.edu NR 117 TC 112 Z9 112 U1 13 U2 80 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-4308 EI 1098-2736 J9 J RES SCI TEACH JI J. Res. Sci. Teach. PD OCT PY 2010 VL 47 IS 8 BP 978 EP 1003 DI 10.1002/tea.20363 PG 26 WC Education & Educational Research SC Education & Educational Research GA 662FX UT WOS:000282793900004 ER PT J AU Cardona, A Valencia, V Garzon, A Montes, C Ojeda, G Ruiz, J Weber, M AF Cardona, A. Valencia, V. Garzon, A. Montes, C. Ojeda, G. Ruiz, J. Weber, M. TI Permian to Triassic I to S-type magmatic switch in the northeast Sierra Nevada de Santa Marta and adjacent regions, Colombian Caribbean: Tectonic setting and implications within Pangea paleogeography SO JOURNAL OF SOUTH AMERICAN EARTH SCIENCES LA English DT Article DE Pangea; Subduction; Accretion; Geochemistry; U-Pb geochronology ID U-PB ZIRCON; GEOLOGIC EVOLUTION; PALEOZOIC ROCKS; SOUTHERN MEXICO; GRANITIC-ROCKS; ANDES; RECONSTRUCTION; GEOCHRONOLOGY; VENEZUELA; GNEISSES AB The Late Paleozoic to Triassic tectonics of northwestern South America have major implications for the understanding of Laurentia-Gondwana interactions that formed Pangea, and the origin of several tectonostratigraphic terranes dispersed by the break-up of this supercontinent during the formation of the Caribbean. Two mylonitic and orthogneissic granitoid suites have been recognized in the northeastern segment of the Sierra Nevada de Santa Marta, the lower Magdalena basin and the Guajira Serranias, within the Caribbean region of Colombia. For the Santa Marta region U/Pb LAM-ICP-MS analysis yielded zircon crystallization ages of 288.1 +/- 4.5 Ma, 276.5 +/- 5,1 Ma and 264.9 +/- 4.0 Ma, related to the magmatic intrusion. Geochemical and modal variations show a compositional spectrum between diorite and granite, whereas LREE enrichment, Ti and Nb anomalies and geochemical discrimination suggest that this granitoid suite was formed within a magmatic arc setting. Inherited zircons suggest that this Early Permian plutonism was formed with the participation of Neoproterozoic and Grenvillian basement proximal to the South American continent. Evidence of a superimposed Early Triassic (ca. 250 Ma) deformational event in Santa Marta, together with a well defined S-type magmatism in the basement rocks from the adjacent lower Magdalena Valley and Guajira Peninsula regions are related to a major shift in the regional tectonic evolution. It's envisioned that this event records either terrane accretion or strong plate coupling during the final stages of Pangea agglutination. Connections with the main Alleghanian-Ouachitan Pangean orogen are precluded due to their timing differences. The plutons temporally and compositionally correlate with an arc found in the northern Andes and Mexican Gondwana terranes, and represent a broader magmatic event formed at the proto-Pacific margin, outside the nucleus of the Laurentia-Gondwana Alleghanian-Oachitan orogens. Evidence of lower temperature recrystallization is probably linked to a younger Late Cretaceous deformational event that reworked the margin during the accretion of the Caribbean arc to the northwest of South America. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Cardona, A.; Montes, C.] Smithsonian Trop Res Inst, Ancon, Panama. [Cardona, A.; Ojeda, G.] Ecopetrol, Inst Colombiano Petr, Piedecuesta, Colombia. [Valencia, V.; Ruiz, J.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. [Garzon, A.] Univ Nacl Colombia, Dept Geociencias, Bogota, Colombia. [Weber, M.] Univ Nacl Colombia, Escuela Geociencias & Medio Ambiente, Medellin, Colombia. RP Cardona, A (reprint author), Smithsonian Trop Res Inst, Ancon, Panama. EM CardonaA@si.edu OI Montes, Camilo/0000-0002-3553-0787 FU ECOPETROL-ICP; INGEOMINAS; INVEMAR; Evolucion Geohistorica de la Sierra Nevada de Santa Marta; Fundacion para el Apoyo de la Investigacion y la Cultura del Banco de la Republica de Colombia [2289]; NSF [EAR-0443387]; International Geological Correlation Program, "Subduction zones of the Caribbean" FX ECOPETROL-ICP, INGEOMINAS and INVEMAR and the Project "Evolucion Geohistorica de la Sierra Nevada de Santa Marta" are acknowledged for their support. Field discussions with F. Colmenares, G. Guzman, and the GEOSEARCH LTDA Sierra Nevada team are fully appreciated. V. Arboleda is acknowledged for help during sampling of the granitoid cores. Discussions with C. Vinasco and M. Ibanez are highly appreciated. J. Duque, M. E. Velazquez and C. A. Salazar are acknowledged for helping with sample preparation. Key suggestions of two anonymous reviewers are highly appreciated. Analytical work was partially supported by a research grant from the Fundacion para el Apoyo de la Investigacion y la Cultura del Banco de la Republica de Colombia, Project 2289. A. Garcia-Casco is kindly acknowledged for access to microprobe analyses. Funding for the Arizona LaserChron Center is provided by NSF EAR-0443387. This is a contribution to Project 546 of the International Geological Correlation Program, "Subduction zones of the Caribbean". NR 72 TC 20 Z9 22 U1 0 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0895-9811 J9 J S AM EARTH SCI JI J. South Am. Earth Sci. PD OCT PY 2010 VL 29 IS 4 SI SI BP 772 EP 783 DI 10.1016/j.jsames.2009.12.005 PG 12 WC Geosciences, Multidisciplinary SC Geology GA 691ZC UT WOS:000285120300003 ER PT J AU Cardona, A Valencia, V Bustamante, C Garcia-Casco, A Ojeda, G Ruiz, J Saldarriaga, M Weber, M AF Cardona, A. Valencia, V. Bustamante, C. Garcia-Casco, A. Ojeda, G. Ruiz, J. Saldarriaga, M. Weber, M. TI Tectonomagmatic setting and provenance of the Santa Marta Schists, northern Colombia: Insights on the growth and approach of Cretaceous Caribbean oceanic terranes to the South American continent SO JOURNAL OF SOUTH AMERICAN EARTH SCIENCES LA English DT Article DE Cretaceous; Caribbean plate; Provenance; Back-arc; U/Pb LAM-ICP-MS; Isotopes; Geochemistry; Colombia ID TRACE-ELEMENT GEOCHEMISTRY; U-PB AGES; CRUSTAL EVOLUTION; BASIN DEVELOPMENT; WESTERN COLOMBIA; TECTONIC HISTORY; VENEZUELA; PLATE; ANDES; CONSTRAINTS AB Metamorphosed volcano-sedimentary rocks accreted to the northern South American continental margin are major vestiges of the Caribbean oceanic plate evolution and its interactions with the continent. Selected whole rock geochemistry, Nd-Sr isotopes and detrital zircon geochronology were obtained in metabasic and metasedimentary rocks from the Santa Marta and San Lorenzo Schists in northernmost Colombia. Trace element patterns are characterized by primitive island arc and MORB signatures. Similarly initial Sr-87/Sr-86-epsilon(Nd) isotopic relations correlate with oceanic arcs and MORB reservoirs, suggesting that the protoliths were formed within a back-arc setting or at the transition between the inta-oceanic arc and the Caribbean oceanic crust. Trace element trends from associated metasedimentary rocks show that the provenance was controlled by a volcanic arc and a sialic continental domain, whereas detrital U/Pb zircons from the Santa Marta Schists and adjacent southeastern metamorphic units show Late Cretaceous and older Mesozoic, Late Paleozoic and Mesoproterozoic sources. Comparison with continental inland basins suggests that this arc-basin is allocthonous to its current position, and was still active by ca. 82 Ma. The geological features are comparable to other arc remnants found in northeastern Colombia and the Netherland Antilles. The geochemical and U/Pb detrital signatures from the metasedimentary rocks suggest that this tectonic domain was already in proximity to the continental margin, in a configuration similar to the modern Antilles or the Kermadec arc in the Pacific. The older continental detritus were derived from the ongoing Andean uplift feeding the intra-oceanic tectonic environment. Cross-cutting relations with granitoids and metamorphic ages suggest that metamorphism was completed by ca. 65 Ma. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Cardona, A.] Smithsonian Trop Res Inst, Ancon, Panama. [Cardona, A.; Ojeda, G.] Inst Colombiano Petr, Piedecuesta, Colombia. [Valencia, V.; Ruiz, J.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. [Bustamante, C.; Saldarriaga, M.] Univ EAFIT, Dept Geol, Medellin, Colombia. [Garcia-Casco, A.] Univ Granada, Dept Mineral & Petrol, E-18071 Granada, Spain. [Weber, M.] Univ Nacl Colombia, Escuela Geociencias & Medio Ambiente, Medellin, Colombia. RP Cardona, A (reprint author), Smithsonian Trop Res Inst, Ancon, Panama. EM CardonaA@si.edu RI Garcia-Casco, Antonio/K-8295-2013; Bustamante, Camilo/N-6273-2015 OI Garcia-Casco, Antonio/0000-0002-8814-402X; Bustamante, Camilo/0000-0002-5527-598X FU ECOPETROL; INVEMAR; INGEOMINAS; Fundacion para el Apoyo de la Investigacion y la Cultura del Banco de la Republica de Colombia [2289]; NSF [EAR-0443387] FX ECOPETROL, INVEMAR and INGEOMINAS are acknowledged for providing support during several phases of this research. Discussions and support from G. Guzman, F. Colmenares and the Geo-search Ltda Sierra Nevada team are highly appreciated. Comments by two anonymous reviewer are highly appreciated Analytical work received support from the Fundacion para el Apoyo de la Investigacion y la Cultura del Banco de la Republica de Colombia, project 2289. Funding for the Arizona LaserChron Center is provided by NSF EAR-0443387. This is a contribution to the IGCP 546: "Subduction zones of the Caribbean." NR 101 TC 15 Z9 16 U1 0 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0895-9811 J9 J S AM EARTH SCI JI J. South Am. Earth Sci. PD OCT PY 2010 VL 29 IS 4 SI SI BP 784 EP 804 DI 10.1016/j.jsames.2009.08.012 PG 21 WC Geosciences, Multidisciplinary SC Geology GA 691ZC UT WOS:000285120300004 ER PT J AU Weber, M Cardona, A Valencia, V Garcia-Casco, A Tobon, M Zapata, S AF Weber, M. Cardona, A. Valencia, V. Garcia-Casco, A. Tobon, M. Zapata, S. TI U/Pb detrital zircon provenance from late cretaceous metamorphic units of the Guajira Peninsula, Colombia: Tectonic implications on the collision between the Caribbean arc and the South American margin SO JOURNAL OF SOUTH AMERICAN EARTH SCIENCES LA English DT Article DE U-Pb detrital zircon provenance analysis; Caribbean arc; South American margin; Arc-continent collision; Guajira Peninsula ID P-T PATHS; EXHUMATION PROCESSES; BASIN DEVELOPMENT; EVOLUTION; PLATE; VENEZUELA; GEOCHRONOLOGY; CONSTRAINTS; SUBDUCTION; ANDES AB Mesozoic metamorphic units exposed along the northern margin of the South American plate record the different stages of subduction evolution or arc-continent collision between the margins of the Caribbean plate and the South American continent. U-Pb detrital zircon geochronology for provenance analysis was carried out on meta-sedimentary rocks of the Etpana formation and metamorphic boulders found within a nearby Tertiary conglomerate, including high-pressure rocks in the Colombian Caribbean. All samples have similar age populations, suggesting that they share a relatively common source and paleogeography. Prominent age peaks include Meso and Paleoproterozoic ages of ca. 1624 Ma and 1315 Ma, Cambrian to Neoproterozoic ages of ca. 630 Ma, 580 Ma and 547 Ma, and less abundant Jurassic and Permian ages of ca. 270 Ma and 160 Ma, which indicate that the South American margin is a major source for the sedimentary protoliths. There are also remnants of younger Cretaceous allocthonous Caribbean arc input at ca. 90-70 Ma. The deposition and metamorphism of these units records the ongoing Late Cretaceous continental subduction of the South American margin within the Caribbean intra-oceanic arc-subduction zone. This gave way to an arc-continent collision between the Caribbean and the South American plates, and sediments with continental signatures were incorporated into the subduction channel and the accretionary wedge. As convergence continued, sediments derived from a mix of South American and arc sources were deposited and included in the collisional wedge up until <71 Ma. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Weber, M.; Tobon, M.; Zapata, S.] Univ Nacl Colombia, Medellin, Colombia. [Cardona, A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Valencia, V.] Univ Arizona, Dept Geosci, Tucson, AZ 85721 USA. [Garcia-Casco, A.] Univ Granada, Dept Geosci, E-18071 Granada, Spain. RP Weber, M (reprint author), Univ Nacl Colombia, Medellin, Colombia. EM mweber@unal.edu.co RI Garcia-Casco, Antonio/K-8295-2013 OI Garcia-Casco, Antonio/0000-0002-8814-402X FU Universidad Nacional de Colombia through DIME [30805975]; Direccion Academica in Medellin; National Science Foundation [EAR-0443387]; Subduction zones of the Caribbean FX Oscar Talavera is acknowledged for discussions and encouragement during field work. Mauricio Ibanez is sincerely acknowledged for its hospitality and continuous help during analytical work at Tucson. The hospitality and help of the LASERCHRON staff is also sincerely acknowledged. Continuous help from Oscar Jaramillo at the Petrography Laboratory, Universidad Nacional de Colombia is greatly appreciated. This research was supported by the Universidad Nacional de Colombia through DIME Grant 30805975 and Direccion Academica in Medellin. Funding for the Arizona Laser-Chron Center is provided by National Science Foundation Grant EAR-0443387. This is a contribution to Project 546 of the International Geological Correlation Program "subduction zones of the Caribbean". NR 81 TC 14 Z9 15 U1 0 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0895-9811 J9 J S AM EARTH SCI JI J. South Am. Earth Sci. PD OCT PY 2010 VL 29 IS 4 SI SI BP 805 EP 816 DI 10.1016/j.jsames.2009.10.004 PG 12 WC Geosciences, Multidisciplinary SC Geology GA 691ZC UT WOS:000285120300005 ER PT J AU Bayona, G Jimenez, G Silva, C Cardona, A Montes, C Roncancio, J Cordani, U AF Bayona, German Jimenez, Giovanny Silva, Cesar Cardona, Agustin Montes, Camilo Roncancio, Jairo Cordani, Umberto TI Paleomagnetic data and K-Ar ages from Mesozoic units of the Santa Marta massif: A preliminary interpretation for block rotation and translations SO JOURNAL OF SOUTH AMERICAN EARTH SCIENCES LA English DT Article DE Santa Marta massif; Vertical-axis rotation; Terrane translation; Caribbean tectonics; Jurassic paleogeography ID NORTHWESTERN SOUTH-AMERICA; COLOMBIAN ANDES; EASTERN CORDILLERA; TECTONIC HISTORY; JURASSIC ROCKS; GEOCHRONOLOGY; NORTHERN; BASIN; VENEZUELA; MODELS AB We report 6 K-Ar ages and paleomagnetic data from 28 sites collected in Jurassic, Lower Cretaceous and Paleocene rocks of the Santa Marta massif, to test previous hypothesis of rotations and translations of this massif, whose rock assemblage differs from other basement-cored ranges adjacent to the Guyana margin. Three magnetic components were identified in this study. A first component has a direction parallel to the present magnetic field and was uncovered in all units (D 352, I = 25.6, k = 57.35, a95 = 5.3, N = 12). A second component was isolated in Cretaceous limestone and Jurassic volcaniclastic rocks (D = 8.8, I = 8.3, k = 24.71, a95 = 13.7, N = 6), and it was interpreted as of Early Cretaceous age. In Jurassic sites with this component, Early Cretaceous K-Ar ages obtained from this and previous studies are interpreted as reset ages. The third component was uncovered in eight sites of Jurassic volcaniclastic rocks, and its direction indicates negative shallow to moderate inclinations and northeastward declinations. K-Ar ages in these sites are of Early (196.5 +/- 4.9 Ma) to early Late Jurassic age (156.6 +/- 8.9 Ma). Due to local structural complexity and too few Cretaceous outcrops to perform a reliable unconformity test, we only used two sites with (1) K-Ar ages, (2) less structural complexity, and (3) reliable structural data for Jurassic and Cretaceous rocks. The mean direction of the Jurassic component is (D = 20.4, I = -18.2, k = 46.9, a95 = 5.1, n = 18 specimens from two sites). These paleomagnetic data support previous models of northward along-margin translations of Grenvillian-cored massifs. Additionally, clockwise vertical-axis rotation of this massif, with respect to the stable craton, is also documented; the sense of rotation is similar to that proposed for the Perija Range and other ranges of the southern Caribbean margin. More data is needed to confirm the magnitudes of rotations and translations. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Bayona, German; Jimenez, Giovanny; Silva, Cesar; Cardona, Agustin; Montes, Camilo] Corp Geol ARES, Bogota, Colombia. [Bayona, German; Silva, Cesar; Cardona, Agustin; Montes, Camilo] Smithsonian Trop Res Inst, Ancon, Panama. [Roncancio, Jairo] Geosearch Ltda, Bogota, Colombia. [Cordani, Umberto] Univ Sao Paulo, Dept Geosci, Sao Paulo, Brazil. RP Bayona, G (reprint author), Corp Geol ARES, Calle 57 24-11 202, Bogota, Colombia. EM gbayona@cgares.org RI Cordani, Umberto/F-3686-2014; OI Cordani, Umberto/0000-0003-4425-5905; Montes, Camilo/0000-0002-3553-0787 FU Ingeominas, Instituto Colombiano del Petroleo and Invemar FX This research was funded by Ingeominas, Instituto Colombiano del Petroleo and Invemar. We acknowledge Ricardo Trindade and Danielle Brant (University of Sao Paulo), and James Channell and Kainian Huang (University of Florida) for assistance and discussion of paleomagnetic data during our work in the Paleomagnetic Laboratories. The field geologist group of Geosearch Ltda contributed to the location of sites during the 2006-2007 field seasons. Johana Casas helped for access to the construction and tunnel of the Rancheria Dam, and Ivan Gutierrez helped in the collection of the samples. We thanks to Georgina Guzman (Invemar) for allowing us the publication of segments of the geologic map of the Sierra Nevada de Santa Marta (Invemar-Ingeominas-Ecopetrol - ICP-Geosearch Ltda, 2007). Comments and suggestions from Roberto Moliza Garza, Victoria Mejia and an anonymous reviewer contributed to improve the presentation of data and content of the manuscript. NR 67 TC 14 Z9 16 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0895-9811 J9 J S AM EARTH SCI JI J. South Am. Earth Sci. PD OCT PY 2010 VL 29 IS 4 SI SI BP 817 EP 831 DI 10.1016/j.jsames.2009.10.005 PG 15 WC Geosciences, Multidisciplinary SC Geology GA 691ZC UT WOS:000285120300006 ER PT J AU Montes, C Guzman, G Bayona, G Cardona, A Valencia, V Jaramillo, C AF Montes, Camilo Guzman, Georgina Bayona, German Cardona, Agustin Valencia, Victor Jaramillo, Carlos TI Clockwise rotation of the Santa Marta massif and simultaneous Paleogene to Neogene deformation of the Plato-San Jorge and Cesar-Rancheria basins SO JOURNAL OF SOUTH AMERICAN EARTH SCIENCES LA English DT Article DE Tectonics; Rotation; Northern Colombia; Santa Marta; Cerrejon; Perija; Plato; San Jorge; Paleomagnetism; Geochronology ID NORTHERN COLOMBIA; SOUTH-AMERICA; TECTONIC SIGNIFICANCE; VENEZUELA; ANDES; EVOLUTION; PERIJA; GNEISSES; SIERRA AB A moderate amount of vertical-axis clockwise rotation of the Santa Marta massif (30 degrees) explains as much as 115 km of extension (stretching of 1.75) along its trailing edge (Plato-San Jorge basin) and up to 56 km of simultaneous shortening with an angular shear of 0.57 along its leading edge (Perija range). Extensional deformation is recorded in the 260 km-wide, fan-shaped Plato-San Jorge basin by a 2-8 km thick, shallowing-upward and almost entirely fine-grained, upper Eocene and younger sedimentary sequence. The simultaneous initiation of shortening in the Cesar-Rancheria basin is documented by Mesozoic strata placed on to lower Eocene syntectonic strata (Tabaco Formation and equivalents) along the northwest-verging, shallow dipping (9-12 degrees to the southeast) and discrete Cerrejon thrust. First-order subsidence analysis in the Plato-San Jorge basin is consistent with crustal stretching values between 1.5 and 2, also predicted by the rigid-body rotation of the Santa Marta massif. The model predicts about 100 km of right-lateral displacement along the Oca fault and 45 km of left-lateral displacement along the Santa Marta-Bucaramanga fault. Clockwise rotation of a rigid Santa Marta massif, and simultaneous Paleogene opening of the Plato-San Jorge basin and emplacement of the Cerrejon thrust sheet would have resulted in the fragmentation of the Cordillera Central-Santa Marta massif province. New U/Pb ages (241 +/- 3 Ma) on granitoid rocks from industry boreholes in the Plato-San Jorge basin confirm the presence of fragments of a now segmented, Late Permian to Early Triassic age, two-mica, granitic province that once spanned the Santa Marta massif to the northernmost Cordillera Central. (C) 2009 Elsevier Ltd. All rights reserved. C1 [Montes, Camilo; Cardona, Agustin; Jaramillo, Carlos] Smithsonian Trop Res Inst, Unit 9100, Dpo, AA 34002 USA. [Guzman, Georgina] Invemar, Cerro Punta Betin, Santa Marta 1016, Colombia. [Bayona, German] Corp Geol Ares, Bogota, Colombia. [Valencia, Victor] Univ Arizona, Arizona Lasechron Ctr, Tucson, AZ USA. RP Montes, C (reprint author), Smithsonian Trop Res Inst, Unit 9100, Box 0948, Dpo, AA 34002 USA. EM montesc@si.edu OI Montes, Camilo/0000-0002-3553-0787 FU Banco de la Republica de Colombia [2289]; NSF [EAR-0443387] FX Banco de la Republica de Colombia partially funded analytical data, Project 2289. Funding for the Arizona LaserChron Center is provided by NSF EAR-0443387. This is a contribution to the IGCP 546: "Subduction zones of the Caribbean". Carbones del Cerrejon Ltd., provided support to students mapping the northern part of the Cesar-Rancheria valley. Thanks to I. Gutierrez for help in field expeditions, to G. Ojeda and C. Vargas for core sampling at the Litoteca Nacional and to N. Hoyos for help in the reconstructions. Backstrip OSX, and Gplates were used in this paper. Comprehensive reviews by F. Roure and an anonymous reviewer helped improve the quality of the manuscript, the authors, however, remain responsible for all errors of fact and interpretation. NR 72 TC 30 Z9 35 U1 0 U2 11 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0895-9811 J9 J S AM EARTH SCI JI J. South Am. Earth Sci. PD OCT PY 2010 VL 29 IS 4 SI SI BP 832 EP 848 DI 10.1016/j.jsames.2009.07.010 PG 17 WC Geosciences, Multidisciplinary SC Geology GA 691ZC UT WOS:000285120300007 ER PT J AU Johnson, KP Clayton, DH Dumbacher, JP Fleischer, RC AF Johnson, Kevin P. Clayton, Dale H. Dumbacher, John P. Fleischer, Robert C. TI The flight of the Passenger Pigeon: Phylogenetics and biogeographic history of an extinct species SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Ectopistes migratorius; Molecular systematics; Ancient DNA; Columbiformes; Doves ID COLUMBICOLA PHTHIRAPTERA; MITOCHONDRIAL; COLUMBIFORMES; NUCLEAR; GENUS; PHILOPTERIDAE; RADIATION; SEQUENCES; BIRDS; AVES AB The human-caused extinction of the Passenger Pigeon (Ectopistes migratorius) is one of the best known and documented of any bird. This event was particularly alarming because the Passenger Pigeon went from being one of the most numerous avian species in the world to extinct in a period of decades, when the last individual died in captivity in a Cincinnati Zoo in 1914. While a great deal of information exists on the likely direct and indirect causes of its demise, as well as information on life-history, the phylogenetic relationships of this species have been subject to considerable speculation. Here we use DNA sequences obtained from museum specimens to resolve the phylogenetic position of this species with respect to other pigeons and doves (Columbiformes). We show that the Passenger Pigeon is not related to the New World mourning doves (Zenaida) as many authors have suggested, but is the sister taxon of all other New World pigeons (Patagioenas). Biogeographic analysis suggests the Passenger Pigeon lineage may have colonized North America from Asia, and subsequently dispersed into South America, leading to a more extensive radiation of New World pigeons. (C) 2010 Published by Elsevier Inc. C1 [Johnson, Kevin P.] Univ Illinois, Illinois Nat Hist Survey, Champaign, IL 61820 USA. [Clayton, Dale H.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Dumbacher, John P.] Calif Acad Sci, San Francisco, CA 94103 USA. [Dumbacher, John P.; Fleischer, Robert C.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. RP Johnson, KP (reprint author), Univ Illinois, Illinois Nat Hist Survey, 1816 S Oak St, Champaign, IL 61820 USA. EM kjohnson@inhs.uiuc.edu FU National Science Foundation [DEB-0107891, DEB-0612938, DEB-0816877] FX The authors thank the Field Museum of Natural History, US National Museum of Natural History, and University of Kansas Museum of Natural History for providing samples of Passenger Pigeon skins. This work was supported by National Science Foundation Grants DEB-0107891 and DEB-0612938 to K.P.J. and DEB-0816877 to D.H.C. NR 21 TC 11 Z9 13 U1 3 U2 60 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD OCT PY 2010 VL 57 IS 1 BP 455 EP 458 DI 10.1016/j.ympev.2010.05.010 PG 4 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 652GY UT WOS:000281992900039 PM 20478386 ER PT J AU Million, ET Werner, N Simionescu, A Allen, SW Nulsen, PEJ Fabian, AC Bohringer, H Sanders, JS AF Million, E. T. Werner, N. Simionescu, A. Allen, S. W. Nulsen, P. E. J. Fabian, A. C. Boehringer, H. Sanders, J. S. TI Feedback under the microscope - I. Thermodynamic structure and AGN-driven shocks in M87 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: individual: M87; intergalactic medium; X-rays: galaxies: clusters ID X-RAY SPECTROSCOPY; ANISOTROPIC THERMAL CONDUCTION; DEEP CHANDRA OBSERVATION; ACTIVE GALACTIC NUCLEI; XMM-NEWTON OBSERVATION; INTRACLUSTER MEDIUM; GALAXY CLUSTERS; SOUND-WAVES; GASEOUS ATMOSPHERE; PERSEUS CLUSTER AB We present the first in a series of papers discussing the thermodynamic properties of M87 and the central regions of the Virgo Cluster in unprecedented detail. Using a deep Chandra exposure (574 ks), we present high-resolution thermodynamic maps created from the spectra of similar to 16 000 independent regions, each with similar to 1000 net counts. The excellent spatial resolution of the thermodynamic maps reveals the dramatic and complex temperature, pressure, entropy and metallicity structure of the system. The 'X-ray arms', driven outwards from M87 by the central active galactic nuclei (AGN), are prominent in the brightness, temperature and entropy maps. Excluding the 'X-ray arms', the diffuse cluster gas at a given radius is strikingly isothermal. This suggests either that the ambient cluster gas, beyond the arms, remains relatively undisturbed by AGN uplift or that conduction in the intracluster medium (ICM) is efficient along azimuthal directions, as expected under action of the heat-flux-driven buoyancy instability (HBI). We confirm the presence of a thick (similar to 40 arcsec or similar to 3 kpc) ring of high-pressure gas at a radius of similar to 180 arcsec (similar to 14 kpc) from the central AGN. We verify that this feature is associated with a classical shock front, with an average Mach number M = 1.25. Another, younger shock-like feature is observed at a radius of similar to 40 arcsec (similar to 3 kpc) surrounding the central AGN, with an estimated Mach number M greater than or similar to 1.2. As shown previously, if repeated shocks occur every similar to 10 Myr, as suggested by these observations, then AGN-driven weak shocks could produce enough energy to offset radiative cooling of the ICM. A high significance enhancement of Fe abundance is observed at radii 350-400 arcsec (27-31 kpc). This ridge is likely formed in the wake of the rising bubbles filled with radio-emitting plasma that drag cool, metal-rich gas out of the central galaxy. We estimate that at least similar to 1.0 x 106 solar masses of Fe has been lifted and deposited at a radius of 350-400 arcsec; approximately the same mass of Fe is measured in the X-ray bright arms, suggesting that a single generation of buoyant radio bubbles may be responsible for the observed Fe excess at 350-400 arcsec. C1 [Million, E. T.; Werner, N.; Simionescu, A.; Allen, S. W.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Million, E. T.; Werner, N.; Simionescu, A.; Allen, S. W.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Nulsen, P. E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fabian, A. C.; Sanders, J. S.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Boehringer, H.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Million, ET (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 382 Via Pueblo Mall, Stanford, CA 94305 USA. EM emillion@stanford.edu OI Sanders, Jeremy/0000-0003-2189-4501; Nulsen, Paul/0000-0003-0297-4493 FU National Aeronautics and Space Administration [PF8-90056, PF9-00070, NAS8-03060]; US Department of Energy [DE-AC02-76SF00515] FX We thank W. R. Forman, C. Jones and E. Churazov for helpful comments and R. G. Morris for computational support. NW and AS were supported by the National Aeronautics and Space Administration through Chandra/Einstein Postdoctoral Fellowship Award Number PF8-90056 and PF9-00070 issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics and Space Administration under contract NAS8-03060. This work was supported in part by the US Department of Energy under contract number DE-AC02-76SF00515. All computational analysis was carried out using the KIPAC XOC compute cluster at Stanford University and the Stanford Linear Accelerator Center (SLAC). NR 57 TC 45 Z9 45 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 1 PY 2010 VL 407 IS 4 BP 2046 EP 2062 DI 10.1111/j.1365-2966.2010.17220.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 651ST UT WOS:000281948100002 ER PT J AU Werner, N Simionescu, A Million, ET Allen, SW Nulsen, PEJ von der Linden, A Hansen, SM Bohringer, H Churazov, E Fabian, AC Forman, WR Jones, C Sanders, JS Taylor, GB AF Werner, N. Simionescu, A. Million, E. T. Allen, S. W. Nulsen, P. E. J. von der Linden, A. Hansen, S. M. Boehringer, H. Churazov, E. Fabian, A. C. Forman, W. R. Jones, C. Sanders, J. S. Taylor, G. B. TI Feedback under the microscope - II. Heating, gas uplift and mixing in the nearest cluster core SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: individual: M87; intergalactic medium; X-rays: galaxies: clusters ID ACTIVE GALACTIC NUCLEI; X-RAY SPECTROSCOPY; COOLING-FLOW CLUSTERS; H-ALPHA FILAMENTS; XMM-NEWTON; INTRACLUSTER MEDIUM; SOUND-WAVES; GASEOUS ATMOSPHERE; CENTAURUS CLUSTER; ELLIPTIC GALAXIES AB Using a combination of deep (574 ks) Chandra data, XMM-Newton high-resolution spectra and optical H alpha+[N ii] images, we study the nature and spatial distribution of the multi-phase plasma in M87. Our results provide direct observational evidence of 'radio-mode' active galactic nuclei (AGN) feedback in action, stripping the central galaxy of its lowest entropy gas and therefore preventing star formation. This low entropy gas was entrained with and uplifted by the buoyantly rising relativistic plasma, forming long 'arms'. A number of arguments suggest that these arms are oriented within 15 degrees-30 degrees of our line-of-sight. The mass of the uplifted gas in the arms is comparable to the gas mass in the approximately spherically symmetric 3.8 kpc core, demonstrating that the AGN has a profound effect on its immediate surroundings. The coolest X-ray emitting gas in M87 has a temperature of similar to 0.5 keV and is spatially coincident with H alpha+[N ii] nebulae, forming a multi-phase medium where the cooler gas phases are arranged in magnetized filaments. We place strong upper limits of 0.06 M(circle dot) yr-1 (at 95 per cent confidence) on the amount of plasma cooling radiatively from 0.5 to 0.25 keV and show that a uniform, volume-averaged heating mechanism could not be preventing the cool gas from further cooling. All of the bright H alpha filaments in M87 appear in the downstream region of the < 3 Myr old shock front, at smaller radii than similar to 0.6 arcmin. We suggest that shocks induce shearing around the filaments, thereby promoting mixing of the cold gas with the ambient hot intra-cluster medium (ICM) via instabilities. By bringing hot thermal particles into contact with the cool, line-emitting gas, mixing can supply the power and ionizing particles needed to explain the observed optical spectra. Furthermore, mixing of the coolest X-ray emitting plasma with the cold optical line-emitting filamentary gas promotes efficient conduction between the two phases, allowing non-radiative cooling which could explain the lack of X-ray gas with temperatures under 0.5 keV. C1 [Werner, N.; Simionescu, A.; Million, E. T.; Allen, S. W.; von der Linden, A.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Werner, N.; Simionescu, A.; Million, E. T.; Allen, S. W.; von der Linden, A.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Nulsen, P. E. J.; Forman, W. R.; Jones, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hansen, S. M.] Univ Calif Santa Cruz, Univ Calif Observ, Santa Cruz, CA 95064 USA. [Hansen, S. M.] Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA. [Boehringer, H.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Churazov, E.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Churazov, E.] Space Res Inst IKI, Moscow 117810, Russia. [Fabian, A. C.; Sanders, J. S.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Taylor, G. B.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. RP Werner, N (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 382 Via Pueblo Mall, Stanford, CA 94305 USA. EM norbertw@stanford.edu RI Churazov, Eugene/A-7783-2013; OI Sanders, Jeremy/0000-0003-2189-4501; Nulsen, Paul/0000-0003-0297-4493 FU National Aeronautics and Space Administration [PF8-90056, PF9-00070, NAS8-03060]; US Department of Energy [DE-AC02-76SF00515]; National Science Foundation [AST-0902010] FX Support for this work was provided by the National Aeronautics and Space Administration through Chandra/Einstein Postdoctoral Fellowship Award Number PF8-90056 and PF9-00070 issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics and Space Administration under contract NAS8-03060. This work was supported in part by the US Department of Energy under contract number DE-AC02-76SF00515. SMH is supported by the National Science Foundation Postdoctoral Fellowship program under award number AST-0902010. NR 78 TC 48 Z9 48 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 1 PY 2010 VL 407 IS 4 BP 2063 EP 2074 DI 10.1111/j.1365-2966.2010.16755.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 651ST UT WOS:000281948100003 ER PT J AU Kipping, DM Tinetti, G AF Kipping, David M. Tinetti, Giovanna TI Nightside pollution of exoplanet transit depths SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: analytical; techniques: photometric; occultations; planetary systems; infrared: general ID EXTRASOLAR GIANT PLANETS; TIME-SERIES PHOTOMETRY; HD 189733B; LIGHT-CURVE; TRANSMISSION SPECTRA; MODEL ATMOSPHERES; MU-M; WATER; PARAMETERS; EMISSION AB Out of the known transiting extrasolar planets, the majority are gas giants orbiting their host star at close proximity. Both theoretical and observational studies support the hypothesis that such bodies emit significant amounts of flux relative to the host star, increasing towards infrared wavelengths. For the dayside of the exoplanet, this phenomenon typically permits detectable secondary eclipses at such wavelengths, which may be used to infer atmospheric composition. In this paper, we explore the effects of emission from the nightside of the exoplanet on the primary transit light curve, which is essentially a self-blend. Allowing for nightside emission, an exoplanet's transit depth is no longer exclusively a function of the ratio-of-radii. The nightside of an exoplanet is emitting flux, and the contrast to the star's emission is of the order of similar to 10-3 for hot Jupiters. Consequently, we show that the transit depth in the mid-infrared will be attenuated due to flux contribution from the nightside emission by similar to 10-4. We show how this effect can be compensated for in the case where exoplanet phase curves have been measured, in particular for HD 189733b. For other systems, it may be possible to make a first-order correction by using temperature estimates of the planet. Unless the effect is accounted for, transmission spectra will also be polluted by nightside emission, and we estimate that a Spitzer broad-band spectrum on a bright target is altered at the 1 Sigma level. Using archived Spitzer measurements, we show that the effect respectively increases the 8.0-mu m and 24.0-mu m transit depths by 1 Sigma and 0.5 Sigma per transit for HD 189733b. Consequently, we estimate that this would be similar to 5-10 Sigma effect for near future James Webb Space Telescope observations. C1 [Kipping, David M.; Tinetti, Giovanna] Univ London Univ Coll, Dept Phys & Astron, London WC1E 6BT, England. [Kipping, David M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kipping, DM (reprint author), Univ London Univ Coll, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM d.kipping@ucl.ac.uk OI Tinetti, Giovanna/0000-0001-6058-6654 FU UCL; Science Technology and Facilities Council (STFC); Harvard-Smithsonian Center for Astrophysics; NASA [NNX08AF23G]; Royal Society FX We thank the anonymous referees for their helpful comments in revising this manuscript. DMK has been supported by UCL, the Science Technology and Facilities Council (STFC) studentships, the Harvard-Smithsonian Center for Astrophysics and NASA grant NNX08AF23G. Special thanks to H. Knutson et al. for kindly providing us with their photometry and I. Ribas for providing limb-darkening coefficients. We would like to thank S. Fossey, M. Swain, J. P. Beaulieu, G. Bakos, G. Vashisht and A. Aylward for their support and discussions in preparing this manuscript. GT is supported by UCL and the Royal Society. NR 48 TC 16 Z9 16 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 1 PY 2010 VL 407 IS 4 BP 2589 EP 2598 DI 10.1111/j.1365-2966.2010.17094.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 651ST UT WOS:000281948100043 ER PT J AU Fietz, J Klose, SM Kalko, EKV AF Fietz, Joanna Klose, Stefan M. Kalko, Elisabeth K. V. TI Behavioural and physiological consequences of male reproductive trade-offs in edible dormice (Glis glis) SO NATURWISSENSCHAFTEN LA English DT Article DE Oxygen consumption; Social thermoregulation; Reproduction small mammal ID YELLOW-PINE CHIPMUNKS; DAILY TORPOR; MYOXUS-GLIS; PLASMA TESTOSTERONE; THYROXINE CYCLES; BODY-TEMPERATURE; SEXUAL-ACTIVITY; METABOLIC-RATE; TESTES SIZE; DORMOUSE AB Testosterone mediates male reproductive trade-offs in vertebrates including mammals. In male edible dormice (Glis glis), reproductivity linked to high levels of testosterone reduces their ability to express torpor, which may be expected to dramatically increase thermoregulatory costs. Aims of this study were therefore to analyse behavioural and physiological consequences of reproductive activity in male edible dormice under ecologically and evolutionary relevant conditions in the field. As we frequently encountered sleeping groups in the field, we hypothesized that social thermoregulation should be an important measure to reduce energy expenditure especially in sexually active male edible dormice. Our results revealed that the occurrence of sleeping groups was negatively influenced by male body mass but not by reproductive status or ambient temperature. In reproductive as in non-reproductive males, the number of individuals huddling together was negatively influenced by their body mass. Thus in general males with a high body mass were sitting in smaller groups than males with a low body mass. However, in reproductive males group size was further negatively affected by ambient temperature and positively by testes size. Thus breeders formed larger sleeping groups at lower ambient temperatures and males with larger testes were found in larger groups than males with smaller testes. Measurements of oxygen consumption demonstrated that grouping behaviour represents an efficient strategy to reduce energy expenditure in edible dormice as it reduced energy requirements by almost 40%. In summary, results of this field study showcase how sexually active male edible dormice may, through behavioural adjustment, counterbalance high thermoregulatory costs associated with reproductive activity. C1 [Fietz, Joanna; Klose, Stefan M.; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Fietz, Joanna] Univ Ulm, Inst Neurobiol, D-89069 Ulm, Germany. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. RP Fietz, J (reprint author), Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM joanna.fietz@uni-ulm.de FU German Research Foundation (DFG) [FI 831/3-1, 831/3-2]; German Wildlife Foundation FX T Kager, T Weis-Dootz, S Schauer and J Schmid helped in many ways with this field project. Financial support provided by the Margarete von Wrangell Programme, the German Research Foundation (DFG, FI 831/3-1; 831/3-2), and the German Wildlife Foundation, all to JF, made this study possible. Comments of four anonymous reviewers improved the manuscript. Our experiments were conducted under licence from the nature conservancy and the animal experiment department of the Regierungsprasidium Tubingen. NR 50 TC 8 Z9 8 U1 3 U2 13 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0028-1042 EI 1432-1904 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD OCT PY 2010 VL 97 IS 10 BP 883 EP 890 DI 10.1007/s00114-010-0704-9 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 653LY UT WOS:000282094100002 PM 20697882 ER PT J AU Harper, SJM Bates, CR Guzman, HM Mair, JM AF Harper, Sarah J. M. Bates, C. Richard Guzman, Hector M. Mair, James M. TI Acoustic mapping of fish aggregation areas to improve fisheries management in Las Perlas Archipelago, Pacific Panama SO OCEAN & COASTAL MANAGEMENT LA English DT Article ID MARINE PROTECTED AREAS; BENTHIC HABITAT; CORAL-REEFS; POPULATION ASSESSMENT; COMMUNITY STRUCTURE; SIDESCAN SONAR; CLASSIFICATION; ASSEMBLAGES; COMPLEXITY; ABUNDANCE AB The purpose of this study was to investigate characterize and map areas of the seabed of Las Perlas Archipelago (LPA) Republic of Panama using swath-bathymetry acoustic sonar techniques and to assess these methods as tools for feeding information into management zoning policy In 2007 the LPA was granted conservation protection under national legislation However detailed management plans are still pending Seabed mapping plays a fundamental role in identifying areas which should be prioritized within the management framework Visual representation of habitat maps provides an effective medium for involving stakeholders in a co-management arena In this survey acoustically mapped areas of the seabed were ground-truthed using a combination of benthic grab samples drop-down video and diver observations The resulting mapped areas were then incorporated into a Geographic Information System (GIS) for further analysis The output was a physical characterization of the seabed at three locations selected for being areas of high rugosity (habitat complexity) and therefore their potential importance as valuable fish aggregation sites The rocky reefs and rhodolith beds identified in this survey represent particularly important fish aggregation and nursery habitats which should be considered priorities for protection under the management plans This survey demonstrated the use of acoustic techniques to spatially resolve topographic features and physical characteristics of the seabed illustrating their potential value as tools for fisheries management and marine reserve zoning in Las Perlas Archipelago and elsewhere (C) 2010 Elsevier Ltd All rights reserved C1 [Mair, James M.] Heriot Watt Univ, Sch Life Sci, Ctr Marine Biodivers & Biotechnol, Edinburgh EH14 4AS, Midlothian, Scotland. [Bates, C. Richard] Univ St Andrews, Dept Earth Sci, St Andrews KY16 9AL, Fife, Scotland. [Guzman, Hector M.] Smithsonian Trop Res Inst, MRC 0580 08, Panama City 03092, Panama. [Harper, Sarah J. M.] Univ British Columbia, AERL, Fisheries Ctr, Vancouver, BC V5Z 1M9, Canada. RP Mair, JM (reprint author), Heriot Watt Univ, Sch Life Sci, Ctr Marine Biodivers & Biotechnol, John Muir Bldg, Edinburgh EH14 4AS, Midlothian, Scotland. OI Bates, Charles Richard/0000-0001-9147-7151 FU UK government s Department for Environment Food and Rural Affairs (DEFRA); St Andrews University; Heriot-Watt University UK; Smithsonian Tropical Research Institute Panama FX We thank the Government of Panama for providing permits to work and collect in the area The authors would like to thank C Guevara R Scott and the crew of R/V Urraca for assisting during the fieldwork We thank our anonymous reviewer for comments on the manuscript Funding for this study was partially provided by the Darwin Initiative a programme of the UK government s Department for Environment Food and Rural Affairs (DEFRA) St Andrews University and Heriot-Watt University UK and the Smithsonian Tropical Research Institute Panama NR 46 TC 5 Z9 6 U1 5 U2 18 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0964-5691 J9 OCEAN COAST MANAGE JI Ocean Coastal Manage. PD OCT PY 2010 VL 53 IS 10 BP 615 EP 623 DI 10.1016/j.ocecoaman.2010.07.001 PG 9 WC Oceanography; Water Resources SC Oceanography; Water Resources GA 682XZ UT WOS:000284437600002 ER PT J AU Minton, MS Mack, RN AF Minton, Mark S. Mack, Richard N. TI Naturalization of plant populations: the role of cultivation and population size and density SO OECOLOGIA LA English DT Article DE Environmental stochasticity; Field trials; Founder population; Invasion; Propagule pressure ID PROPAGULE PRESSURE; ENVIRONMENTAL STOCHASTICITY; RAINFALL VARIABILITY; UNITED-STATES; BIOLOGY; EXTINCTION; INVASIONS; DYNAMICS; CONSERVATION; GRASSLAND AB Field experimentation is required to assess the effects of environmental stochasticity on small immigrant plant populations-a widely understood but largely unexplored aspect of predicting any species' likelihood of naturalization and potential invasion. Cultivation can mitigate this stochasticity, although the outcome for a population under cultivation nevertheless varies enormously from extinction to persistence. Using factorial experiments, we investigated the effects of population size, density, and cultivation (irrigation) on the fate of founder populations for four alien species with different life history characteristics (Echinochloa frumentacea, Fagopyrum esculentum, Helianthus annuus, and Trifolium incarnatum) in eastern Washington, USA. The fate of founder populations was highly variable within and among the 3 years of experimentation and illustrates the often precarious environment encountered by plant immigrants. Larger founder populations produced more seeds (P < 0.001); the role of founder population size, however, differed among years. Irrigation resulted in higher percent survival (P < 0.001) and correspondingly larger net reproductive rate (R (0); P < 0.001). But the minimum level of irrigation for establishment, R (0) > 1, differed among years and species. Sowing density did not affect the likelihood of establishment for any species. Our results underscore the importance of environmental stochasticity in determining the fate of founder populations and the potential of cultivation and large population size in countering the long odds against naturalization. Any implementation of often proposed post-immigration field trials to assess the risk of an alien species becoming naturalized, a requisite step toward invasion, will need to assess different sizes of founder populations and the extent and character of cultivation (intentional or unintentional) that the immigrants might receive. C1 [Minton, Mark S.; Mack, Richard N.] Washington State Univ, Sch Biol Sci, Pullman, WA 99164 USA. RP Minton, MS (reprint author), Smithsonian Environm Res Ctr, Edgewater, MD 21307 USA. EM mintonm@si.edu OI Minton, Mark/0000-0002-9439-4930 FU Betty Higinbotham Trust; Washington State University FX We thank R. A. Black, R. M. Hannan, C. L. Kinter, E. L. Minton, R. R. Pattison and R. B. Pratt for their support and comments throughout the project. R. Colautti provided helpful comments on an earlier draft of the manuscript. K. Tetrich and the USDA Plant Introduction Facility in Central Ferry, Washington provided essential help. Finally, we are grateful to numerous volunteers, who assisted with the implementation and harvesting of these experiments. This research was supported by grants to M. S. M. from the Betty Higinbotham Trust and a Natural Resources Conservation Grant at Washington State University. Experiments reported in this work comply with the current laws of the United States of America. NR 62 TC 14 Z9 14 U1 1 U2 30 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD OCT PY 2010 VL 164 IS 2 BP 399 EP 409 DI 10.1007/s00442-010-1667-4 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 650PB UT WOS:000281860700012 PM 20532919 ER PT J AU Puerta-Pinero, C AF Puerta-Pinero, Carolina TI Changes in riparian forest composition along a sedimentation rate gradient SO PLANT ECOLOGY LA English DT Article DE Landscape ecology; Pre-dispersal seed predation; Post-dispersal seed predation; Quercus ilex; Recruitment; Spatial analysis ID POSTDISPERSAL SEED PREDATION; SPATIAL-PATTERNS; QUERCUS-ILEX; JANZEN-CONNELL; LANDSCAPE ECOLOGY; SUS-SCROFA; RECRUITMENT; DISPERSAL; OAK; ESTABLISHMENT AB Riparian forests are highly valued for maintaining water quality through the retention of sediments and nutrients. They also provide some of the most diverse and species-rich habitats in the world. What is largely unknown, however, is how sediment deposition affects plant community composition in these forests. The objective of this study was to examine changes in plant community composition across a gradient of increasing rates of sedimentation in riparian forests in the southeastern Coastal Plain, USA. Seventeen plots were established within riparian forests receiving between 0 and 5.5 cm year(-1) of sediment deposits. Species density and biomass estimates were collected annually from 2002 to 2006 for overstory and mid-story plant species within each plot. Percent cover and nested frequency of understory plant species were determined annually during 2004-2006. Measures of community composition in the understory, mid-story, and overstory layers of forests were compared to changes in environmental factors associated with increased sedimentation. In the understory, annual, exotic, and upland species had higher importance values in plots receiving high sediment deposition. The densities of shade-intolerant and N-fixing species in the mid-story also increased with increasing sedimentation rates. Increased overstory mortality was associated with high sedimentation rates, though increases in understory light levels in these gaps were not the main driver of understory species changes. Edaphic factors, such as soil texture, moisture, and temperature, were significantly correlated to species composition in all three forest layers, suggesting that changes in soil physical structure due to sedimentation may drive community-level changes in these forests. C1 [Puerta-Pinero, Carolina] Univ Granada, Dept Ecol, Fac Ciencias, Granada 18071, Spain. RP Puerta-Pinero, C (reprint author), Smithsonian Trop Res Inst, Unit 9100, Box 0948, DPO, AA 34002 USA. EM puertac@si.edu RI Puerta Pinero, Carolina/B-3186-2012 OI Puerta Pinero, Carolina/0000-0002-0584-7548 FU Spanish Ministry of Science and Education [AP2003-344]; University of Granada [REN2003-07048, CSD2008-00040]; CTFC; Fundacion Caja Madrid FX Jose Maria Gomez Reyes kindly supervised all the intellectual processes of this manuscript. Manuel Martinez helped in constructing all the enclosures in the lab. Abby Britten nicely revised the English writing. Gustavo P. Bornemann, Seila Lopez, Carla Steffler and Alba Puerta Pinero gave vital assistance during the field work. The headquarters of the Sierra Nevada National Park and Jardin Botanico de la Cortijuela offered support for working in the field. Several anonymous referees and JM Espelta deeply improved preliminary versions of this manuscript. This study was supported by the Spanish Ministry of Science and Education via the FPU fellowship AP2003-344, and financial project REN2003-07048 and CSD2008-00040 and postdoctoral fellowships from the University of Granada, CTFC and Fundacion Caja Madrid. NR 56 TC 13 Z9 13 U1 4 U2 21 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1385-0237 J9 PLANT ECOL JI Plant Ecol. PD OCT PY 2010 VL 210 IS 2 BP 213 EP 224 DI 10.1007/s11258-010-9750-9 PG 12 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 642ZE UT WOS:000281259700002 ER PT J AU Henry, TJ AF Henry, Thomas J. TI NEW PLANT BUG (HEMIPTERA: HETEROPTERA: MIRIDAE) RECORDS FOR WEST VIRGINIA SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Insecta; Hemiptera; Heteroptera; Miridae; West Virginia; USA; new records ID NORTH-AMERICA HETEROPTERA; EASTERN-UNITED-STATES; PILOPHORINI HETEROPTERA; PHYLINAE; REVISION; FIEBER; GENUS; HAHN AB Thirty-two species of Miridae are recorded for the first time from West Virginia. With an additional six species reported in the literature and two subsequent synonymies since the 1983 "Annotated List..." by Wheeler, Mason, and Henry, 283 species of Miridae are now known from the state. The new records include six species in the subfamily Bryocorinae, two in Cylapinae, two in Deraeocorinae, twelve in Mirinae, seven in Orthotylinae, and three in Phylinae. Locality information, specific dates, associated host data, and number of specimens and sex are given for each species. Names used in the previous 1983 list are updated. C1 Smithsonian Inst, Natl Museum Nat Hist, Systemat Entomol Lab, Inst Plant Sci,ARS,USDA, Washington, DC 20013 USA. RP Henry, TJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Systemat Entomol Lab, Inst Plant Sci,ARS,USDA, POB 37012, Washington, DC 20013 USA. EM thomas.henry@ars.usda.gov NR 49 TC 1 Z9 1 U1 1 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2010 VL 112 IS 4 BP 490 EP 499 DI 10.4289/0013-8797.112.4.490 PG 10 WC Entomology SC Entomology GA 708IN UT WOS:000286355600002 ER PT J AU Wheeler, AG Evans, GA Vandenberg, NJ AF Wheeler, A. G., Jr. Evans, Gregory A. Vandenberg, Natalia J. TI PSEUDOCOCCUS SACCHARICOLA TAKAHASHI (HEMIPTERA: PSEUDOCOCCIDAE) IN THE BRITISH VIRGIN ISLANDS: FIRST WESTERN HEMISPHERE RECORDS, WITH RECORDS OF A CO-OCCURRING LADY BEETLE, HYPERASPIS SCUTIFERA (MULSANT) (COLEOPTERA: COCCINELLIDAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Insecta; yellowish sugarcane mealybug; adventive species; insect detection; new records; new synonymy; West Indies ID DISPERSAL; INSECTS; INDIES; NORTH; PESTS AB Pseudococcus saccharicola Takahashi was collected on Guana Island, and nearby Beef Island and Tortola, in the British Virgin islands (BVI). The records are the first in the Western Hemisphere for this potentially important Old World pest of sugarcane and certain other graminoid crops. Host plants on Guana were Chloris barbata Sw. (swollen fingergrass), C. radiata (L.) (radiate fingergrass), Cynodon dactylon L. (bermudagrass), and Saccharum officinarum L. (sugarcane). A probable mealybug predator associated with colonies of P. saccharicola on all three islands was the hyperaspidine coccinellid Hyperaspis scutifera (Mulsant), previously recorded in the West Indies only from the Leeward Antilles (Curacao). Both the mealybug and lady beetle are considered adventive in the BVI. Diagnoses and illustrations of both species are provided to facilitate their recognition. Hyperaspis sanctaeritae Dobzhansky, 1941, described from Arizona, USA, is proposed (by N.J.V.) as a junior synonym of H. scutifera (Mulsant 1850). C1 [Wheeler, A. G., Jr.] Clemson Univ, Dept Entomol Soils & Plant Sci, Clemson, SC 29634 USA. [Evans, Gregory A.] USDA APHIS, Systemat Entomol Lab, PSI, BARC W, Beltsville, MD 20705 USA. [Vandenberg, Natalia J.] Smithsonian Inst, Natl Museum Nat Hist, Systemat Entomol Lab, PSI,USDA ARS, Washington, DC 20013 USA. RP Wheeler, AG (reprint author), Clemson Univ, Dept Entomol Soils & Plant Sci, Clemson, SC 29634 USA. EM awhlr@clemson.edu; Gregory.A.Evans@aphis.usda.gov; Natalia.Vandenberg@ars.usda.gov NR 53 TC 0 Z9 0 U1 1 U2 2 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2010 VL 112 IS 4 BP 565 EP 575 DI 10.4289/0013-8797.112.4.565 PG 11 WC Entomology SC Entomology GA 708IN UT WOS:000286355600011 ER PT J AU Loinard, L Rodriguez, LF Gomez, L Canto, J Raga, AC Goodman, AA Arce, HG AF Loinard, L. Rodriguez, L. F. Gomez, L. Canto, J. Raga, A. C. Goodman, A. A. Arce, H. G. TI A REASSESSMENT OF THE KINEMATICS OF PV CEPHEI BASED ON ACCURATE PROPER MOTION MEASUREMENTS SO REVISTA MEXICANA DE ASTRONOMIA Y ASTROFISICA LA English DT Article DE astrometry; ISM: individual (PV Cep); ISM: jets and outflows; stars: pre-main sequence ID SYSTEM IRAS 16293-2422; YOUNG STELLAR-SYSTEM; MULTIPLE SYSTEM; RADIO-SOURCES; SIDE WIND; JET; ORION; STAR; EJECTION; REGION AB We present two Very Large Array observations of the pre-main-sequence star PV Cephei, taken with a separation of 10.5 years. These data show that the proper motions of this star are mu(alpha) cos delta = +10.9 +/- 3.0 mas yr(-1); mu(alpha) = +0.2 +/- 1.8 mas yr(-1), very similar to those -previously known- of HD 200775, the B2Ve star that dominates the illumination of the nearby reflection nebula NGC 7023. This result suggests that PV Cephei is not a rapidly moving runaway star as suggested by previous studies. The large velocity of PV Cephei had been inferred from the systematic eastward displacement of the bisectors of successive pairs of Herbig Haro knots along its flow. These systematic shifts might instead result from an intrinsic asymmetry in the ejection mechanisms, or in the distribution of the circumstellar material. C1 [Loinard, L.; Rodriguez, L. F.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Canto, J.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Raga, A. C.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico. [Gomez, L.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Goodman, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Arce, H. G.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. RP Loinard, L (reprint author), Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Apdo Postal 3-72 Xangari, Morelia 58089, Michoacan, Mexico. EM l.loinard@crya.unam.mx; l.rodriguez@crya.unam.mx; lgo-mez@mpifr.de; raga@nucleares.unam.mx; agoodman@cfa.harvard.edu; hector.arce@yale.edu RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 FU DGAPA, Universidad Nacional Autonoma de Mexico; International Max Planck Research School (IMPRS); Conacyt (Mexico) FX LFR, LL, JC and ACE acknowledge the support of DGAPA, Universidad Nacional Autonoma de Mexico, and of Conacyt (Mexico). L. G. was supported for this research through a stipend from the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne. This research has made use of the SIMBAD database, operated. at CDS, Strasbourg, France. NR 34 TC 0 Z9 0 U1 0 U2 0 PU UNIV NACIONAL AUTONOMA MEXICO, INST DE ASTRONOMIA PI MEXICO CITY PA APDO POSTAL 70-264, MEXICO CITY 04510, MEXICO SN 0185-1101 J9 REV MEX ASTRON ASTR JI Rev. Mex. Astron. Astrofis. PD OCT PY 2010 VL 46 IS 2 BP 367 EP 375 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 659WC UT WOS:000282596800016 ER PT J AU Holman, MJ Fabrycky, DC Ragozzine, D Ford, EB Steffen, JH Welsh, WF Lissauer, JJ Latham, DW Marcy, GW Walkowicz, LM Batalha, NM Jenkins, JM Rowe, JF Cochran, WD Fressin, F Torres, G Buchhave, LA Sasselov, DD Borucki, WJ Koch, DG Basri, G Brown, TM Caldwell, DA Charbonneau, D Dunham, EW Gautier, TN Geary, JC Gilliland, RL Haas, MR Howell, SB Ciardi, DR Endl, M Fischer, D Furesz, G Hartman, JD Isaacson, H Johnson, JA MacQueen, PJ Moorhead, AV Morehead, RC Orosz, JA AF Holman, Matthew J. Fabrycky, Daniel C. Ragozzine, Darin Ford, Eric B. Steffen, Jason H. Welsh, William F. Lissauer, Jack J. Latham, David W. Marcy, Geoffrey W. Walkowicz, Lucianne M. Batalha, Natalie M. Jenkins, Jon M. Rowe, Jason F. Cochran, William D. Fressin, Francois Torres, Guillermo Buchhave, Lars A. Sasselov, Dimitar D. Borucki, William J. Koch, David G. Basri, Gibor Brown, Timothy M. Caldwell, Douglas A. Charbonneau, David Dunham, Edward W. Gautier, Thomas N., III Geary, John C. Gilliland, Ronald L. Haas, Michael R. Howell, Steve B. Ciardi, David R. Endl, Michael Fischer, Debra Fueresz, Gabor Hartman, Joel D. Isaacson, Howard Johnson, John A. MacQueen, Phillip J. Moorhead, Althea V. Morehead, Robert C. Orosz, Jerome A. TI Kepler-9: A System of Multiple Planets Transiting a Sun-Like Star, Confirmed by Timing Variations SO SCIENCE LA English DT Article ID EXTRA-SOLAR PLANETS; SUPER-EARTHS; SOLID EXOPLANETS; HARPS SEARCH; MASS; RESONANCES; DYNAMICS; MOTION; PERFORMANCE; STABILITY AB The Kepler spacecraft is monitoring more than 150,000 stars for evidence of planets transiting those stars. We report the detection of two Saturn-size planets that transit the same Sun-like star, based on 7 months of Kepler observations. Their 19.2- and 38.9-day periods are presently increasing and decreasing at respective average rates of 4 and 39 minutes per orbit; in addition, the transit times of the inner body display an alternating variation of smaller amplitude. These signatures are characteristic of gravitational interaction of two planets near a 2: 1 orbital resonance. Six radial-velocity observations show that these two planets are the most massive objects orbiting close to the star and substantially improve the estimates of their masses. After removing the signal of the two confirmed giant planets, we identified an additional transiting super-Earth-size planet candidate with a period of 1.6 days. C1 [Holman, Matthew J.; Fabrycky, Daniel C.; Ragozzine, Darin; Latham, David W.; Fressin, Francois; Torres, Guillermo; Buchhave, Lars A.; Sasselov, Dimitar D.; Charbonneau, David; Geary, John C.; Fueresz, Gabor; Hartman, Joel D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ford, Eric B.; Moorhead, Althea V.; Morehead, Robert C.] Univ Florida, Gainesville, FL 32611 USA. [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Welsh, William F.; Orosz, Jerome A.] San Diego State Univ, San Diego, CA 92182 USA. [Lissauer, Jack J.; Jenkins, Jon M.; Rowe, Jason F.; Borucki, William J.; Koch, David G.; Caldwell, Douglas A.; Haas, Michael R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Lissauer, Jack J.] Stanford Univ, Stanford, CA 94305 USA. [Marcy, Geoffrey W.; Walkowicz, Lucianne M.; Basri, Gibor; Isaacson, Howard] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Batalha, Natalie M.] San Jose State Univ, San Jose, CA 95192 USA. [Jenkins, Jon M.; Caldwell, Douglas A.] SETI Inst, Mountain View, CA 94043 USA. [Cochran, William D.; Endl, Michael; MacQueen, Phillip J.] Univ Texas Austin, Austin, TX 78712 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Brown, Timothy M.] Global Telescope, Las Cumbres Observ, Goleta, CA 93117 USA. [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Fischer, Debra] Yale Univ, New Haven, CT 06510 USA. [Brown, Timothy M.] Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA. RP Holman, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mholman@cfa.harvard.edu RI Steffen, Jason/A-4320-2013; Ragozzine, Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014; OI Caldwell, Douglas/0000-0003-1963-9616; Buchhave, Lars A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA's Science Mission Directorate; NASA [NCC2-1390]; NSF [0707203] FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. We acknowledge NASA Cooperative Agreement NCC2-1390. D. C. F. acknowledges support from the Michelson Fellowship, supported by NASA and administered by the NASA Exoplanet Science Institute. This material is based on work supported by the NSF under grant no. 0707203. This work is based, in part, on observations obtained at the W. M. Keck Observatory, which is operated by the Univ. of California and the California Institute of Technology. Some of the observations in this paper were obtained at Kitt Peak National Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy under cooperative agreement with the NSF. J.F.R. is a NASA postdoctoral program fellow. We are grateful to N. Haghighipour for many helpful comments and suggestions. NR 44 TC 213 Z9 213 U1 1 U2 11 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD OCT 1 PY 2010 VL 330 IS 6000 BP 51 EP 54 DI 10.1126/science.1195778 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 656KW UT WOS:000282334500030 PM 20798283 ER PT J AU Clough, GW AF Clough, G. Wayne TI Show and Tell SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Clough, GW (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOC PI WASHINGTON PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD OCT PY 2010 VL 41 IS 6 BP 28 EP 28 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 655IP UT WOS:000282243500008 ER PT J AU Wakelam, V Smith, IWM Herbst, E Troe, J Geppert, W Linnartz, H Oberg, K Roueff, E Agundez, M Pernot, P Cuppen, HM Loison, JC Talbi, D AF Wakelam, V. Smith, I. W. M. Herbst, E. Troe, J. Geppert, W. Linnartz, H. Oeberg, K. Roueff, E. Agundez, M. Pernot, P. Cuppen, H. M. Loison, J. C. Talbi, D. TI Reaction Networks for Interstellar Chemical Modelling: Improvements and Challenges SO SPACE SCIENCE REVIEWS LA English DT Review DE Astrochemistry; Reaction rate coefficients; Gas-phase chemistry; Grain-surface chemistry; Chemical modelling; Uncertainty propagation; Sensitivity analysis ID MOLECULAR-HYDROGEN FORMATION; GAS-PHASE REACTIONS; PHOTOCHEMICAL KINETICS UNCERTAINTIES; ENVELOPE SURROUNDING IRC+10216; NEUTRAL-NEUTRAL REACTIONS; MONTE-CARLO SIMULATIONS; ADIABATIC CHANNEL MODEL; ELEY-RIDEAL MECHANISM; GRAPHITE SURFACE; TITANS ATMOSPHERE AB We survey the current situation regarding chemical modelling of the synthesis of molecules in the interstellar medium. The present state of knowledge concerning the rate coefficients and their uncertainties for the major gas-phase processes-ion-neutral reactions, neutral-neutral reactions, radiative association, and dissociative recombination-is reviewed. Emphasis is placed on those key reactions that have been identified, by sensitivity analyses, as 'crucial' in determining the predicted abundances of the species observed in the interstellar medium. These sensitivity analyses have been carried out for gas-phase models of three representative, molecule-rich, astronomical sources: the cold dense molecular clouds TMC-1 and L134N, and the expanding circumstellar envelope IRC +10216. Our review has led to the proposal of new values and uncertainties for the rate coefficients of many of the key reactions. The impact of these new data on the predicted abundances in TMC-1 and L134N is reported. Interstellar dust particles also influence the observed abundances of molecules in the interstellar medium. Their role is included in gas-grain, as distinct from gas-phase only, models. We review the methods for incorporating both accretion onto, and reactions on, the surfaces of grains in such models, as well as describing some recent experimental efforts to simulate and examine relevant processes in the laboratory. These efforts include experiments on the surface-catalyzed recombination of hydrogen atoms, on chemical processing on and in the ices that are known to exist on the surface of interstellar grains, and on desorption processes, which may enable species formed on grains to return to the gas-phase. C1 [Wakelam, V.] Univ Bordeaux, Observ Aquitain Sci Univers, F-33271 Floirac, France. [Wakelam, V.] CNRS, Lab Astrophys Bordeaux, UMR 5804, F-33271 Floriac, France. [Smith, I. W. M.] Univ Chem Labs, Cambridge CB2 1EW, England. [Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Troe, J.] Univ Gottingen, Inst Phys Chem, D-37077 Gottingen, Germany. [Troe, J.] Max Planck Inst Biophys Chem, D-37077 Gottingen, Germany. [Geppert, W.] Univ Stockholm, Dept Phys, S-10691 Stockholm, Sweden. [Linnartz, H.; Oeberg, K.; Cuppen, H. M.] Leiden Univ, Sackler Lab Astrophys, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Oeberg, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Roueff, E.] Univ Paris 07, F-92195 Meudon, France. [Roueff, E.] CNRS, Observ Paris, LUTH, UMR 8102, F-92195 Meudon, France. [Agundez, M.] Observ Paris, LUTH, F-92190 Meudon, France. [Pernot, P.] Univ Paris 11, Chim Phys Lab, UMR 8000, F-91405 Orsay, France. [Pernot, P.] CNRS, F-91405 Orsay, France. [Loison, J. C.] Univ Bordeaux 1, Inst Mol Sci, CNRS, UMR 5255, F-33405 Talence, France. [Talbi, D.] Univ Montpellier 2, GRAAL, CNRS, UMR 5024, F-34095 Montpellier, France. RP Wakelam, V (reprint author), Univ Bordeaux, Observ Aquitain Sci Univers, BP 89, F-33271 Floirac, France. EM wakelam@obs.u-bordeaux1.fr RI PERNOT, Pascal/C-2643-2008; Cuppen, Herma/F-9729-2015; Agundez, Marcelino/I-5369-2012; OI PERNOT, Pascal/0000-0001-8586-6222; Cuppen, Herma/0000-0003-4397-0739; Agundez, Marcelino/0000-0003-3248-3564; Wakelam, Valentine/0000-0001-9676-2605 FU French program PCMI; Center for the Chemistry of the Universe (NSF, US); Royal Society FX We acknowledge the "International Space Science Institute" for hosting the meetings of the international team "A new generation of databases for interstellar chemical modeling in preparation for HSO and ALMA". We would also like to thank the following people who took part in one or both of the ISSI meetings but did not contribute a section to this report: Nathalie Carrasco, Prof. Ewine van Dishoeck, Prof. Dieter Gerlich, Eric Hebrard, Liv Hornekaer, Andrew Markwick, Prof. Tom Millar, Anton Vasyunin. V.W. thanks Astrid Bergeat for discussions about N + NO reaction. V.W., JC.L. and D. T. thank the French program PCMI for partial funding of this work. E. H. wishes to thank the Center for the Chemistry of the Universe (NSF, US) for support of his program in chemical kinetics. VW and IWMS thank the Royal Society for a grant to facilitate their co-operation. NR 200 TC 104 Z9 104 U1 6 U2 58 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD OCT PY 2010 VL 156 IS 1-4 BP 13 EP 72 DI 10.1007/s11214-010-9712-5 PG 60 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 726WX UT WOS:000287758700002 ER PT J AU Dorr, LJ Wiersema, JH AF Dorr, Laurence J. Wiersema, John H. TI Typification of names of American species of vascular plants proposed by Linnaeus and based on Loefling's Iter Hispanicum (1758) SO TAXON LA English DT Article DE Nicolaus Joseph von Jacquin; neotype; nomenclature; lectotype; Linnaean names; Pehr Loefling; Iter Hispanicum AB Neotypes are proposed for the names of ten species of American plants that Linnaeus based in whole or in part on descriptions in Loefling's Iter Hispanicum:Allionia incarnata, Allionia violacea, Ayenia tomentosa, Byttneria scabra, Krameria ixine, Lecythis ollaria, Moniera trifolia, Viola arborea, Viola calceolaria, and Viola oppositifolia. Lectotypes are proposed for the names of six species of American plants that Linnaeus based in whole or in part on descriptions in the same work: Ayenia magna, Cecropia peltata, Ellisia acuta, jussiaea pubescens, Loranthus occidentalis, and Spermacoce strigosa. A neotype also is proposed for a Jacquin name, Hybanthus havanensis, which Linnaeus renamed as Viola hybanthus. We also argue that Laetia americana is neotypified by the type applied to the illegitimate name Laetia apetala. C1 [Dorr, Laurence J.] Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, Washington, DC 20013 USA. [Wiersema, John H.] USDA ARS, Natl Germplasm Resources Lab, Beltsville Agr Res Ctr BARC W, Beltsville, MD 20705 USA. RP Dorr, LJ (reprint author), Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, MRC 166,POB 37012, Washington, DC 20013 USA. EM dorrl@si.edu NR 35 TC 7 Z9 8 U1 0 U2 1 PU INT ASSOC PLANT TAXONOMY-IAPT PI BRATISLAVA PA C/O INST BOTANY, SLOVAK ACAD SCIENCES DUBRAVSKA CESTA 9, SK-845 23 BRATISLAVA, SLOVAKIA SN 0040-0262 EI 1996-8175 J9 TAXON JI Taxon PD OCT PY 2010 VL 59 IS 5 BP 1571 EP 1577 PG 7 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 663XZ UT WOS:000282924800021 ER PT J AU Pretzer, WS AF Pretzer, William S. TI Structures of Change in the Mechanical Age: Technological Innovation in the United States, 1790-1865 SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 [Pretzer, William S.] Smithsonian Inst, Natl Museum African Amer Hist & Culture, Washington, DC 20560 USA. RP Pretzer, WS (reprint author), Smithsonian Inst, Natl Museum African Amer Hist & Culture, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD OCT PY 2010 VL 51 IS 4 BP 1026 EP 1028 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA 685YN UT WOS:000284664100021 ER PT J AU Litaker, RW Vandersea, MW Faust, MA Kibler, SR Nau, AW Holland, WC Chinain, M Holmes, MJ Tester, PA AF Litaker, R. Wayne Vandersea, Mark W. Faust, Maria A. Kibler, Steven R. Nau, Amy W. Holland, William C. Chinain, Mireille Holmes, Michael J. Tester, Patricia A. TI Global distribution of ciguatera causing dinoflagellates in the genus Gambierdiscus SO TOXICON LA English DT Article DE Biogeography; CFP; Ciguatera fish poisoning; Gambierdiscus australes; G. belizeanus; G. caribaeus; G. carpenteri; G. carolinianus; G. pacificus; G. polynesiensis; G. ruetzleri; G. toxicus; G. yasumotoi; Maitotoxin; Monitoring; Phylogeny; Ribotype ID WATER-SOLUBLE TOXIN; JACK CARANX-LATUS; FRENCH-POLYNESIA; INDIAN-OCEAN; CARIBBEAN CIGUATOXINS; FUKUYO DINOPHYCEAE; FLORIDA KEYS; CORAL-REEF; TOXICITY; FISH AB Dinoflagellates in the genus Gambierdiscus produce toxins that bioaccumulate in tropical and sub-tropical fishes causing ciguatera fish poisoning (CFP). Little is known about the diversity and distribution of Gambierdiscus species, the degree to which individual species vary in toxicity, and the role each plays in causing CFP. This paper presents the first global distribution of Gambierdiscus species. Phylogenetic analyses of the existing isolates indicate that five species are endemic to the Atlantic (including the Caribbean/West Indies and Gulf of Mexico), five are endemic to the tropical Pacific, and that two species. Gambierdiscus carpenteri and Gambierdiscus caribaeus are globally distributed. The differences in Gambierdiscus species composition in the Atlantic and Pacific correlated with structural differences in the ciguatoxins reported from Atlantic and Pacific fish. This correlation supports the hypothesis that Gambierdiscus species in each region produce different toxin suites. A literature survey indicated a >100-fold variation in toxicity among species compared with a 2 to 9-fold within species variation due to changing growth conditions. These observations suggest that CFP events are driven more by inherent differences in species toxicity than by environmental modulation. How variations in species toxicity may affect the development of an early warning system for CFP is discussed. Published by Elsevier Ltd. C1 [Litaker, R. Wayne; Vandersea, Mark W.; Kibler, Steven R.; Nau, Amy W.; Holland, William C.; Tester, Patricia A.] NOAA, NOS, Ctr Coastal Fisheries & Habitat Res, Beaufort, NC 28516 USA. [Faust, Maria A.] Smithsonian Inst, United States Natl Herbarium, Dept Bot, Suitland, MD 20746 USA. [Chinain, Mireille] Inst Louis Malarde, Lab Microalgues Tox, Papeete 98713, Tahiti, Fr Polynesia. [Holmes, Michael J.] Queensland Dept Environm & Resource Management, Brisbane, Qld 4001, Australia. RP Litaker, RW (reprint author), NOAA, NOS, Ctr Coastal Fisheries & Habitat Res, 101 Pivers Isl Rd, Beaufort, NC 28516 USA. EM wayne.litaker@noaa.gov FU Smithsonian Institution; Smithsonian Institution Hunterdon Oceanographic Research Endowment; NOAA FX We thank Dr. Klaus Rutzler, National Museum of Natural History, Smithsonian Institution for his long-term support of the research program in Belize from which we have benefited greatly. Special thanks to Michael Carpenter and Bertol Pfeiffer for logistic support. Dr. Clement Lewsey from NOAA's International Programs Office provided critical support for the sampling efforts in the Puerto Rico region. Partial support for the research also came from grants provided by the Smithsonian Institution Caribbean Coral Reef Ecosystem Program (CCRE), the Smithsonian Institution Hunterdon Oceanographic Research Endowment and NOAA program funds. This is contribution number 844 of the Caribbean Coral Reef Ecosystems Program. We thank Paula Whitfield, Christine Addison, Brian Degan, Roldan Munoz, John Burke, Dave Cerino, Michael Dowgiallo, Wilson Freshwater, David Johnson, Brett Harrison, Doug Kesling, William Lee, Roger Mays, James Morris, Brandon Puckett, Sherry Reed, and Brad Teer for assisting in sample collection from the Caribbean and West Indies. NR 137 TC 73 Z9 79 U1 6 U2 41 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0041-0101 J9 TOXICON JI Toxicon PD OCT PY 2010 VL 56 IS 5 SI SI BP 711 EP 730 DI 10.1016/j.toxicon.2010.05.017 PG 20 WC Pharmacology & Pharmacy; Toxicology SC Pharmacology & Pharmacy; Toxicology GA 645XN UT WOS:000281499600008 PM 20561539 ER PT J AU Hoffman, RN Dailey, P Hopsch, S Ponte, RM Quinn, K Hill, EM Zachry, B AF Hoffman, Ross N. Dailey, Peter Hopsch, Susanna Ponte, Rui M. Quinn, Katherine Hill, Emma M. Zachry, Brian TI An Estimate of Increases in Storm Surge Risk to Property from Sea Level Rise in the First Half of the Twenty-First Century SO WEATHER CLIMATE AND SOCIETY LA English DT Article AB Sea level is rising as the World Ocean warms and ice caps and glaciers melt. Published estimates based on data from satellite altimeters, beginning in late 1992, suggest that the global mean sea level has been rising on the order of 3 mm yr(-1). Local processes, including ocean currents and land motions due to a variety of causes, modulate the global signal spatially and temporally. These local signals can be much larger than the global signal, and especially so on annual or shorter time scales. Even increases on the order of 10 cm in sea level can amplify the already devastating losses that occur when a hurricane-driven storm surge coincides with an astronomical high tide. To quantify the sensitivity of property risk to increasing sea level, changes in expected annual losses to property along the U. S. Gulf and East Coasts are calculated as follows. First, observed trends in sea level rise from tide gauges are extrapolated to the year 2030, and these changes are interpolated to all coastal locations. Then a 10 000-yr catalog of simulated hurricanes is used to define critical wind parameters for each event. These wind parameters then drive a parametric time-evolving storm surge model that accounts for bathymetry, coastal geometry, surface roughness, and the phase of the astronomical tide. The impact of the maximum storm surge height on a comprehensive inventory of commercial and residential property is then calculated, using engineering models that take into account the characteristics of the full range of construction types. Average annual losses projected to the year 2030 are presented for regions and key states and are normalized by aggregate property value on a zip code by zip code basis. Comparisons to the results of a control run reflecting the risk today quantify the change in risk per dollar of property on a percentage basis. Increases in expected losses due to the effect of sea level rise alone vary by region, with increases of 20% or more being common. Further sensitivity tests quantify the impact on the risk of sea level rise plus additional factors, such as changes in hurricane frequency and intensity as a result of rising sea surface temperatures. C1 [Hoffman, Ross N.; Hopsch, Susanna; Ponte, Rui M.; Quinn, Katherine] Atmospher & Environm Res Inc, Lexington, MA 02421 USA. [Dailey, Peter; Hopsch, Susanna; Zachry, Brian] AIR Worldwide Corp, Boston, MA USA. [Hill, Emma M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hoffman, RN (reprint author), Atmospher & Environm Res Inc, 131 Hartwell Ave, Lexington, MA 02421 USA. EM rhoffman@aer.com RI Hill, Emma/B-7037-2011; OI Hill, Emma/0000-0003-0231-5818; Ponte, Rui/0000-0001-7206-6461 FU NASA [NNX07AM77G]; NSF [OCE-0961507] FX Tide gauge data used in this study came from the PSMSL and NOAA (NOAA 2007). E. M. Hill and R. M. Ponte were supported by the NASA Grant NNX07AM77G. Additional support at AER was provided by NSF Grant OCE-0961507. NR 48 TC 10 Z9 14 U1 2 U2 10 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 1948-8327 EI 1948-8335 J9 WEATHER CLIM SOC JI Weather Clim. Soc. PD OCT PY 2010 VL 2 IS 4 BP 271 EP 293 DI 10.1175/2010WCAS1050.1 PG 23 WC Environmental Studies; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA V22HT UT WOS:000208267000003 ER PT J AU Mathis, WN Marinoni, L AF Mathis, Wayne N. Marinoni, Luciane TI A review of Diphuia (Diptera: Ephydridae) with description of two new species from southern Brazil SO ZOOLOGIA LA English DT Review DE Neotropical; New World; shore-fly; taxonomy ID CRESSON DIPTERA; REVISION AB The species of Diphuia Cresson, 1944 are reviewed with an emphasis on the fauna from southern Brazil, where two new species have been discovered and herein are described: Diphuia antonina sp. nov. and Diphuia grandis sp. nov. All known species are placed into two species groups (the anomala and nitida groups), which are characterized, and a key to these species is included. To facilitate identification of species of this uncommon genus, we have included diagnoses of the genus and tribe Hecamedini and have also provided an annotated key to New World genera in the tribe and to the known species of Diphuia. We have also provided illustrations of structures of the male terminalia of all included species. The species from southern Brazil, including the new ones, are illustrated. C1 [Mathis, Wayne N.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Marinoni, Luciane] Univ Fed Parana, Dept Zool, BR-81531980 Curitiba, Parana, Brazil. RP Mathis, WN (reprint author), Smithsonian Inst, Dept Entomol, NHB 169,POB 37012, Washington, DC 20013 USA. EM mathisw@si.edu; lmarinoni@ufpr.br RI Marinoni, Luciane /C-5720-2013 FU CNPq [401609/2009-0] FX Recent field work in Brazil (December 2009-June 2010) that resulted in the vast majority of specimens studied in this paper was supported by a grant from CNPq (Visiting Researcher/Process 401609/2009-0), which we gratefully acknowledge and thank. We thank Dianne Mathis for helping with all aspects of the production of this paper, especially the field work in Brazil. We also thank A. Bernardo Carvalho and his lab (Elisa, Monica, Susana) for hosting us while conducting field work along the coast of Sao Paulo. NR 17 TC 2 Z9 2 U1 0 U2 2 PU SOC BRASILEIRA ZOOLOGIA, UNIV FEDERAL PARANA PI CURITIBA PA CAIXA POSTAL 19020, CURITIBA, PARANA 81531-980, BRAZIL SN 1984-4670 J9 ZOOLOGIA-CURITIBA JI Zoologia PD OCT PY 2010 VL 27 IS 5 BP 803 EP 812 DI 10.1590/S1984-46702010000500017 PG 10 WC Zoology SC Zoology GA 699LX UT WOS:000285666000017 ER PT J AU Baeza, JA AF Baeza, J. Antonio TI Molecular systematics of peppermint and cleaner shrimps: phylogeny and taxonomy of the genera Lysmata and Exhippolysmata (Crustacea: Caridea: Hippolytidae) SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Exhippolysmata; hermaphrodite; Hippolytidae; Lysmata; Merguia ID PROTANDRIC SIMULTANEOUS HERMAPHRODITISM; SEX ALLOCATION; MARINE SHRIMP; GENUS LYSMATA; EVOLUTION; DECAPODA; DNA AB Shrimps from the ecologically diverse genera Lysmata and Exhippolysmata are rare among marine invertebrates because they are protandric simultaneous hermaphrodites: shrimps initially mature and reproduce solely as males, and later in life become functional simultaneous hermaphrodites. Considerable progress on the reproductive ecology of members from these two genera has been achieved during the last decade. However, several outstanding issues of systematic nature remain to be addressed. Here, a molecular phylogeny of these two genera was used to examine the overall evolutionary relationship within and between species and genera, and to answer various questions related to the systematic status of several species. The present phylogenetic analysis, including 53 sequences and 26 species of Lysmata and Exhippolysmata, indicates that semiterrestrial shrimps from the genus Merguia represent the sister group to a second natural clade composed by shrimps from the genera Lysmata and Exhippolysmata. Also, the phylogenetic analysis confirmed that the genus Lysmata is paraphyletic, and includes the genus Exhippolysmata, as noted in a preliminary study. The tree partially supports the separation of species with or without a developed accessory branch into two different genera or subgenera ( i. e. Lysmata and Hippolysmata having a well- developed accessory branch, or not, respectively). The genetic distance between the cleaner shrimps Lysmata amboinensis and Lysmata grabhami was smaller than has been observed between other sister species. On the other hand, the topology of the tree indicates that these two entities are reciprocally monophyletic. Thus, this latter result, together with minor but constant differences in the colour pattern reported for these two entities, indicates that there is no reason to stop treating them as different valid species. This study enabled the long overdue resolution of standing taxonomic questions in shrimps from the genera Lysmata and Exhippolysmata. In the future, this phylogeny will help to reveal the conditions favouring the origins of several behavioural and morphological novelties in these unique shrimps. c 2010 The Linnean Society of London, Zoological Journal of the Linnean Society, 2010, 160, 254-265. doi: 10.1111/ j. 1096-3642.2009.00605. x C1 [Baeza, J. Antonio] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Baeza, J. Antonio] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Baeza, J. Antonio] Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Larrondo 1281, Coquimbo, Chile. RP Baeza, JA (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. EM baezaa@si.edu OI Baeza, Juan Antonio/0000-0002-2573-6773 FU STRI; SMSFP; National Geographic Society, USA FX Many thanks to Bill Hoffman from the Smithsonian Marine Ecosystems Exhibit (SMEE), Valerie Paul, Raphael Ritson-Williams, and Julie Piraino from the Smithsonian Marine Station at Fort Pierce (SMSFP), Narissa Bax from New Zealand, Luis Ignacio Vilchis and William A. Newman from the Scripps Institution of Oceanography (SIO), University of California at San Diego, Juan Bolanos, Jesus Enrique Hernandez, and Regulo Lopez from the Universidad de Oriente (UDO), Boca del Rio, Venezuela, Adriane A. Braga from the Universidade Estadual Paulista (UNESP), Botucatu, Brazil, Arthur Anker from the University of Florida, Gainsville, USA, Carla Piantonni from the National Museum of Natural History, Washington D.C., USA, Arcadio Ortiz from the Smithsonian Tropical Research Institute (STRI), Panama, Nancy Voss from the University of Miami and Fernando Alvarez from the Universidad Nacional Autonoma de Mexico (UNAM), Mexico City, for their help during the different steps of specimen collection and loans. My sincere appreciation goes to Juan Bolanos for inviting me to dictate a course on the Behaviour of Marine Invertebrates at Isla Margarita, where a great portion of this manuscript was written. Especial thanks to Jeff Hunt and Lee Weigt at the Laboratory of Analytical Biology, NMNH, Washington D.C. for their logistical support. JAB thanks the support from a STRI Marine Postdoctoral Fellowship and a SMSFP Postdoctoral Fellowship. This study was partial funded by a National Geographic Research Grant from the National Geographic Society, USA. Raymond T. Bauer (University of Louisiana at Lafayette, USA) and Christoph Schubart (Regensburg Universitat, Germany) helped improve preliminary versions of this manuscript. The comments of two anonymous reviewers substantially improved this manuscript. This is contribution number 790 of the Smithsonian Marine Station at Fort Pierce. NR 45 TC 17 Z9 17 U1 1 U2 10 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4082 EI 1096-3642 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD OCT PY 2010 VL 160 IS 2 BP 254 EP 265 DI 10.1111/j.1096-3642.2009.00605.x PG 12 WC Zoology SC Zoology GA 656HY UT WOS:000282321100002 ER PT J AU Mah, C Nizinski, M Lundsten, L AF Mah, Christopher Nizinski, Martha Lundsten, Lonny TI Phylogenetic revision of the Hippasterinae (Goniasteridae; Asteroidea): systematics of deep sea corallivores, including one new genus and three new species SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Review DE Arctic; deep-sea coral; deep-sea echinoderm; Evoplosoma; feeding biology; Hippasteria; onshore-offshore; phylogeny; taxonomy ID CORAL LOPHELIA-PERTUSA; ATLANTIC; FAUNA; ECHINODERMATA; CALIFORNIA; STARFISH; GULF; BIOGEOGRAPHY; MEGAFAUNA; HABITAT AB The Hippasterinae is a subfamily within the Goniasteridae, consisting of five genera and 26 species, which occur in cold-water settings ranging from subtidal to abyssal depths. All known genera were included in a cladistic analysis resulting in two most parsimonious trees, supporting the Hippasterinae as monophyletic. Our review supports Sthenaster emmae gen. et sp. nov. as a new genus and species from the tropical Atlantic and two new Evoplosoma species, Evoplosoma claguei sp. nov. and Evoplosoma voratus sp. nov. from seamounts in the North Pacific. Hippasteria caribaea is reassigned to the genus Gilbertaster, which previously contained a single Pacific species. Our analysis supports Evoplosoma as a derived deep water lineage relative to its continental-shelf, shallow water sister taxa. The genus Hippasteria contains approximately 15 widely distributed, but similar-looking species, which occur in the northern and southern hemispheres. Except for Gilbertaster, at least one species in each genus has been observed or is inferred to prey on deep-sea corals, suggesting that this lineage is important to the conservation of deep-sea coral habitats. The Hippasterinae shares several morphological similarities with Circeaster and Calliaster, suggesting that they may be related. c 2010 The Linnean Society of London, Zoological Journal of the Linnean Society, 2010, 160, 266- 301. doi: 10.1111/ j. 1096-3642.2010.00638.x C1 [Mah, Christopher] Natl Museum Nat Hist, Smithsonian Inst Invertebrate Zool, Washington, DC 20013 USA. [Nizinski, Martha] Natl Museum Nat Hist, Natl Marine Fisheries Serv, Natl Systemat Lab, Washington, DC 20013 USA. [Lundsten, Lonny] Monterey Bay Aquarium Res Inst, Video Lab, Moss Landing, CA 95039 USA. RP Mah, C (reprint author), Natl Museum Nat Hist, Smithsonian Inst Invertebrate Zool, MRC 163,POB 37012, Washington, DC 20013 USA. EM mahch@si.edu FU NOAA Office of Ocean Exploration; NMNH; NSF [0631245] FX The authors of this study are indebted to Cynthia Gust Ahearn (deceased), collection manager for the NMNH Echinodermata Collection, and Cheryl Ames (UNCW, National Systematics Laboratory, NMFS) for curatorial assistance. Steve Cairns, curator of Coelenterates, NMNH identified the gorgonian spicules. Dave Pawson, Paul Greenhall, and Linda Ward (NMNH) provided additional logistical and technical support. Mary Catherine Boyett (MCZ) prepared the loan of type material from MCZ. David Clague and James Barry (MBARI) made recent collections available. Support for sampling off the south-eastern coast of the US was provided by grants from NOAA Office of Ocean Exploration (S.W. Ross, lead Investigator). The science party, the crew of the R/V Seward Johnson, and the pilots of the Johnson Sea Link are greatly acknowledged for assistance with collection of western Atlantic material. We thank the crew of the R/V Western Flyer and the pilots of the ROV Tiburon for their assistance with Pacific collections as well as the David and Lucile Packard Foundation for support of MBARI. Michael Carlson prepared the map for Atlantic collections in Figure 1. We also thank Christopher Kelley, Hawaiian Undersea Research Laboratory, for making in situ observations available to us. Daniel Blake, University of Illinois at Urbana Champaign, Andy Gale, University of Portsmouth, and an anonymous reviewer provided useful comments that improved the manuscript. C. Mah was supported by the United States Antarctic Research Program at the NMNH and NSF OPP Postdoctoral Fellows grant # 0631245. NR 131 TC 25 Z9 30 U1 1 U2 13 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0024-4082 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD OCT PY 2010 VL 160 IS 2 BP 266 EP 301 DI 10.1111/j.1096-3642.2010.00638.x PG 36 WC Zoology SC Zoology GA 656HY UT WOS:000282321100003 ER PT J AU Zeugin, F Potvin, C Jansa, J Scherer-Lorenzen, M AF Zeugin, F. Potvin, C. Jansa, J. Scherer-Lorenzen, M. TI Is tree diversity an important driver for phosphorus and nitrogen acquisition of a young tropical plantation? SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Biodiversity and ecosystem functioning; Nutrient use efficiency; Sardinilla; Panama; Tropical tree plantations; Resource complementarity; Environmental heterogeneity ID NUTRIENT-USE EFFICIENCY; MIXED-SPECIES PLANTATIONS; COSTA-RICA; HUMID TROPICS; ABOVEGROUND BIOMASS; FOREST PLANTATIONS; ECOSYSTEM FUNCTION; SECONDARY FORESTS; SOIL INTERACTIONS; PURE PLANTATIONS AB Many tropical plantations in Central America are monocultures of fast growing, mostly exotic species such as a teak, eucalypts and pines. This has been perceived as a problem for ecosystem stability, pest control, local biodiversity and long-term nutrient availability. In our study, we followed the effects of increasing tree diversity (1,3 and 6 native species) on aboveground nitrogen (N) and phosphorus (P) pools in a young experimental biodiversity plantation (central Panama) over two subsequent years. Our results show a positive but not consistent net effect of biodiversity on the N and P pools, mainly explained by the complementarity effect. N and P use efficiencies strongly varied among the investigated tree species and the species richness gradient. Anacardium excelsum and Luehea seemannii were associated with higher N and P use efficiencies while Hura crepitans and Tabebuia rosea were less efficient in aboveground biomass production per unit N or P. Tree species tended to have lower P use efficiencies in the intermediate diversity level compared to monocultures and six-species mixtures. Although the environmental conditions explained a large part of the variation in the N and P pools (58%) in our experiment, we argue that incorporating tree mixtures in the management can bring additional benefits and improve tree growth and nutrient uptake as compared to the monocultures. (C) 2010 Elsevier B.V. All rights reserved. C1 [Zeugin, F.; Scherer-Lorenzen, M.] ETH, Inst Plant Anim & Agroecosyst Sci, CH-8092 Zurich, Switzerland. [Potvin, C.] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Potvin, C.] Smithsonian Trop Res Inst, Panama City, Panama. [Jansa, J.] Swiss Fed Inst Technol, Inst Plant Anim & Agroecosyst Sci, CH-8315 Lindau, Switzerland. RP Zeugin, F (reprint author), ETH, Inst Plant Anim & Agroecosyst Sci, CH-8092 Zurich, Switzerland. EM fabienne.zeugin@ipw.agrl.ethz.ch RI Jansa, Jan/H-3161-2014 OI Jansa, Jan/0000-0002-0331-1774 FU Swiss National Science Foundation [3100A0-110031/1] FX We are grateful to Iliana & Jose Monteza, Felipe Rodriguez and all the field workers in Sardinilla for great help in the field. We would like to thank Ben Turner (Smithsonian Tropical Research Institute, Panama), Karin Sorgel, Annika Lenz and Thomas Flura (ETH Zurich, Switzerland) for help with the lab analyses. Information on the elevation and the slope inclination of each plot and the plantation map were kindly provided by Sebastian Wolf (ETH Zurich, Switzerland). Authors are indebted to Yvonne Oelmann (Johannes Gutenberg University Mainz, Germany) who accepted to share raw data on stem N and P concentrations with us, and to Else Bunemann and Thomas Seitlinger (ETH Zurich and University Zurich, Switzerland), who kindly provided part of the soil phosphorus data. We also like to thank Christian Schob and Petr Smilauer for their advices on the statistical analyses. We are grateful to the Smithsonian Tropical Research Institute, Panama, and especially to Raineldo Urriola, for constant support. This research was made possible by a grant of the Swiss National Science Foundation (3100A0-110031/1). NR 67 TC 17 Z9 17 U1 2 U2 41 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD SEP 30 PY 2010 VL 260 IS 9 BP 1424 EP 1433 DI 10.1016/j.foreco.2010.07.020 PG 10 WC Forestry SC Forestry GA 670WO UT WOS:000283458600002 ER PT J AU Arvidson, RE Bell, JF Bellutta, P Cabrol, NA Catalano, JG Cohen, J Crumpler, LS Marais, DJD Estlin, TA Farrand, WH Gellert, R Grant, JA Greenberger, RN Guinness, EA Herkenhoff, KE Herman, JA Iagnemma, KD Johnson, JR Klingelhofer, G Li, R Lichtenberg, KA Maxwell, SA Ming, DW Morris, RV Rice, MS Ruff, SW Shaw, A Siebach, KL de Souza, PA Stroupe, AW Squyres, SW Sullivan, RJ Talley, KP Townsend, JA Wang, A Wright, JR Yen, AS AF Arvidson, R. E. Bell, J. F., III Bellutta, P. Cabrol, N. A. Catalano, J. G. Cohen, J. Crumpler, L. S. Marais, D. J. Des Estlin, T. A. Farrand, W. H. Gellert, R. Grant, J. A. Greenberger, R. N. Guinness, E. A. Herkenhoff, K. E. Herman, J. A. Iagnemma, K. D. Johnson, J. R. Klingelhoefer, G. Li, R. Lichtenberg, K. A. Maxwell, S. A. Ming, D. W. Morris, R. V. Rice, M. S. Ruff, S. W. Shaw, A. Siebach, K. L. de Souza, P. A. Stroupe, A. W. Squyres, S. W. Sullivan, R. J. Talley, K. P. Townsend, J. A. Wang, A. Wright, J. R. Yen, A. S. TI Spirit Mars Rover Mission: Overview and selected results from the northern Home Plate Winter Haven to the side of Scamander crater SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID THERMODYNAMIC BEHAVIOR; THEORETICAL PREDICTION; AQUEOUS ELECTROLYTES; HIGH PRESSURES; TEMPERATURES; DEPOSITS; LIFE AB This paper summarizes Spirit Rover operations in the Columbia Hills, Gusev crater, from sol 1410 (start of the third winter campaign) to sol 2169 (when extrication attempts from Troy stopped to winterize the vehicle) and provides an overview of key scientific results. The third winter campaign took advantage of parking on the northern slope of Home Plate to tilt the vehicle to track the sun and thus survive the winter season. With the onset of the spring season, Spirit began circumnavigating Home Plate on the way to volcanic constructs located to the south. Silica-rich nodular rocks were discovered in the valley to the north of Home Plate. The inoperative right front wheel drive actuator made climbing soil-covered slopes problematical and led to high slip conditions and extensive excavation of subsurface soils. This situation led to embedding of Spirit on the side of a shallow, 8 m wide crater in Troy, located in the valley to the west of Home Plate. Examination of the materials exposed during embedding showed that Spirit broke through a thin sulfate-rich soil crust and became embedded in an underlying mix of sulfate and basaltic sands. The nature of the crust is consistent with dissolution and precipitation in the presence of soil water within a few centimeters of the surface. The observation that sulfate-rich deposits in Troy and elsewhere in the Columbia Hills are just beneath the surface implies that these processes have operated on a continuing basis on Mars as landforms have been shaped by erosion and deposition. C1 [Arvidson, R. E.; Catalano, J. G.; Greenberger, R. N.; Guinness, E. A.; Lichtenberg, K. A.; Shaw, A.; Siebach, K. L.; Wang, A.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Bell, J. F., III; Rice, M. S.; Squyres, S. W.; Sullivan, R. J.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Bellutta, P.; Estlin, T. A.; Herman, J. A.; Maxwell, S. A.; Stroupe, A. W.; Talley, K. P.; Townsend, J. A.; Wright, J. R.; Yen, A. S.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Cabrol, N. A.; Marais, D. J. Des] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Cabrol, N. A.] SETI Inst, Mountain View, CA USA. [Cohen, J.] Honeybee Robot Spacecraft Mech Corp, New York, NY 10001 USA. [Crumpler, L. S.] New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. [Farrand, W. H.] Space Sci Inst, Boulder, CO 80301 USA. [Gellert, R.] Univ Guelph, Dept Phys, Guelph, ON N1G 2W1, Canada. [Grant, J. A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Herkenhoff, K. E.; Johnson, J. R.] US Geol Survey, Flagstaff, AZ 86001 USA. [Iagnemma, K. D.] MIT, Dept Mech Engn, Cambridge, MA 02139 USA. [Klingelhoefer, G.] Johannes Gutenberg Univ Mainz, Inst Anorgan & Analyt Chem, D-55099 Mainz, Germany. [Li, R.] Ohio State Univ, Dept Civil & Environm Engn & Geodet Sci, Columbus, OH 43210 USA. [Ming, D. W.; Morris, R. V.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Ruff, S. W.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [de Souza, P. A.] CSIRO, Informat & Commun Technol Ctr, Hobart, Tas 7001, Australia. RP Arvidson, RE (reprint author), Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. EM arvidson@rsmail.wustl.edu RI de Souza, Paulo/B-8961-2008; Centre, TasICT/D-1212-2011; Catalano, Jeffrey/A-8322-2013; Johnson, Jeffrey/F-3972-2015; OI de Souza, Paulo/0000-0002-0091-8925; Catalano, Jeffrey/0000-0001-9311-977X; Siebach, Kirsten/0000-0002-6628-6297; Greenberger, Rebecca/0000-0003-1583-0261 FU NASA FX We thank the capable team of engineers and scientists at the Jet Propulsion Laboratory and elsewhere who made the Spirit mission possible. We also thank support from NASA for the science team. NR 34 TC 40 Z9 41 U1 1 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD SEP 30 PY 2010 VL 115 AR E00F03 DI 10.1029/2010JE003633 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 658TF UT WOS:000282511600003 ER PT J AU Yeates, AR Mackay, DH van Ballegooijen, AA Constable, JA AF Yeates, A. R. Mackay, D. H. van Ballegooijen, A. A. Constable, J. A. TI A nonpotential model for the Sun's open magnetic flux SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID CORONAL MASS EJECTIONS; GLOBAL SOLAR CORONA; LONG-TERM VARIATION; ACTIVE-REGION 10953; LARGE-SCALE CORONA; FILAMENT CHANNELS; EVOLUTION MODEL; SOURCE SURFACE; FIELD MODEL; INTERPLANETARY AB Measurements of the interplanetary magnetic field (IMF) over several solar cycles do not agree with computed values of open magnetic flux from potential field extrapolations. The discrepancy becomes greater around solar maximum in each cycle when the IMF can be twice as strong as predicted by the potential field model. Here we demonstrate that this discrepancy may be resolved by allowing for electric currents in the low corona (below 2.5R(circle dot)). We present a quasi-static numerical model of the large-scale coronal magnetic evolution, which systematically produces these currents through flux emergence and shearing by surface motions. The open flux is increased by 75%-85% at solar maximum, but only 25% at solar minimum, bringing it in line with estimates from IMF measurements. The additional open flux in the nonpotential model arises through inflation of the magnetic field by electric currents, with superimposed fluctuations due to coronal mass ejections. The latter are modeled by the self-consistent ejection of twisted magnetic flux ropes. C1 [Yeates, A. R.] Univ Dundee, Div Math, Dundee DD1 4HN, Scotland. [Yeates, A. R.; van Ballegooijen, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mackay, D. H.; Constable, J. A.] Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. RP Yeates, AR (reprint author), Univ Dundee, Div Math, Dundee DD1 4HN, Scotland. EM anthony@maths.dundee.ac.uk; duncan@mcs.st-and.ac.uk RI Yeates, Anthony/D-1338-2014 OI Yeates, Anthony/0000-0002-2728-4053 FU UK/STFC; NASA [NNM07AB07C, NNX08AW53]; Royal Society FX We thank the referees for constructive suggestions. A.R.Y. and D.H.M. acknowledge financial support from the UK/STFC, and A.R.Y. was also supported by NASA contract NNM07AB07C to SAO (where much of this work was undertaken). Simulations used the UKMHD parallel computer in St. Andrews (SRIF/STFC), and support from a Royal Society research grant to D.H.M. The visit of J.A.C. to SAO was supported by NASA grant NNX08AW53. Synoptic magnetogram data from NSO/Kitt Peak were produced cooperatively by NSF/NOAO, NASA/GSFC, and NOAA/SEL and made publicly accessible on the World Wide Web. The OMNI IMF data were obtained from the GSFC/SPDF OMNIWeb interface at http://omniweb.gsfc.nasa.gov. NR 62 TC 22 Z9 22 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD SEP 29 PY 2010 VL 115 AR A09112 DI 10.1029/2010JA015611 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 658TU UT WOS:000282513100004 ER PT J AU Liu, CX Liu, Y Cai, ZN Gao, ST Bian, JC Liu, XO Chance, K AF Liu, Chuanxi Liu, Yi Cai, Zhaonan Gao, Shouting Bian, Jianchun Liu, Xiong Chance, Kelly TI Dynamic formation of extreme ozone minimum events over the Tibetan Plateau during northern winters 1987-2001 SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID MADDEN-JULIAN OSCILLATION; TROPOSPHERIC OZONE; LOWER STRATOSPHERE; CLIMATOLOGY; TROPOPAUSE; HEMISPHERE; PACIFIC; HOLES AB Wintertime extreme ozone minima in the total column ozone over the Tibetan Plateau (TP) between 1978 and 2001 are analyzed using observations from the Total Ozone Mapping Spectrometer (TOMS), Global Ozone Monitoring Experiment (GOME), and reanalysis data from both National Centers for Environmental Prediction and European Centre for Medium-Range Weather Forecasts. Results show that total column ozone reduction in nine persistent (lasting for at least 2 days) and four transient events can be substantially attributed to ozone reduction in the upper troposphere and lower stratosphere region (below 25 km). This reduction is generally caused by uplift of the local tropopause and northward transport of tropical ozone-poor air associated with an anomalous anticyclone in the upper troposphere. These anticyclonic anomalies are closely related to anomalous tropical deep convective heating, which is, however, not necessarily phase locked with the tropical Madden-Julian Oscillation as in our earlier case study. Considering stratospheric processes, the selected 13 events can be combined into nine independent events. Moreover, five of the nine independent events, especially the persistent events, are coupled with contributions from stratospheric dynamics between 25 and 40 km, i.e., 15%-40% derived from GOME observations for events in November 1998, February 1999, and December 2001. On the basis of these events, stratospheric column ozone reduction over the TP region can be attributed to the dynamics (development and/or displacement) of the two main stratospheric systems, namely, the polar vortex and the Aleutian High. The effect of a "low-ozone pocket" inside the Aleutian High on the total column ozone in East Asia requires further study. C1 [Liu, Chuanxi; Liu, Yi; Cai, Zhaonan; Bian, Jianchun] Chinese Acad Sci, Inst Atmospher Phys, Key Lab Middle Atmosphere & Global Environm Obser, Beijing 100029, Peoples R China. [Liu, Xiong; Chance, Kelly] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gao, Shouting] Chinese Acad Sci, Inst Atmospher Phys, LACS, Beijing 100029, Peoples R China. [Liu, Xiong] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. [Liu, Chuanxi; Cai, Zhaonan] Chinese Acad Sci, Grad Univ, Beijing 100029, Peoples R China. RP Liu, CX (reprint author), Chinese Acad Sci, Inst Atmospher Phys, Key Lab Middle Atmosphere & Global Environm Obser, Beijing 100029, Peoples R China. RI Liu, Xiong/P-7186-2014; OI Liu, Xiong/0000-0003-2939-574X; Chance, Kelly/0000-0002-7339-7577 FU National Basic Research Program of China [2010CB428604]; National Science Foundation of China [40633015]; Dragon 2 Programme [5311]; NASA; Smithsonian Institution FX This work was funded by the National Basic Research Program of China (grant 2010CB428604), National Science Foundation of China (grant 40633015), and the Dragon 2 Programme (ID: 5311). We thank the European Space Agency and the German Aerospace Center for their ongoing cooperation in the GOME program. The meteorological analysis was kindly provided by ECMWF and NCEP. Research at SAO was funded by NASA and the Smithsonian Institution. NR 46 TC 6 Z9 7 U1 0 U2 17 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP 24 PY 2010 VL 115 AR D18311 DI 10.1029/2009JD013130 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 656ID UT WOS:000282321800001 ER PT J AU France, K McCray, R Heng, K Kirshner, RP Challis, P Bouchet, P Crotts, A Dwek, E Fransson, C Garnavich, PM Larsson, J Lawrence, SS Lundqvist, P Panagia, N Pun, CSJ Smith, N Sollerman, J Sonneborn, G Stocke, JT Wang, LF Wheeler, JC AF France, Kevin McCray, Richard Heng, Kevin Kirshner, Robert P. Challis, Peter Bouchet, Patrice Crotts, Arlin Dwek, Eli Fransson, Claes Garnavich, Peter M. Larsson, Josefin Lawrence, Stephen S. Lundqvist, Peter Panagia, Nino Pun, Chun S. J. Smith, Nathan Sollerman, Jesper Sonneborn, George Stocke, John T. Wang, Lifan Wheeler, J. Craig TI Observing Supernova 1987A with the Refurbished Hubble Space Telescope SO SCIENCE LA English DT Article ID BALMER-DOMINATED SHOCKS; SNR 1987A; REVERSE SHOCK; CIRCUMSTELLAR RING; OPTICAL-EMISSION; LINE EMISSION; SN-1987A; ULTRAVIOLET; REMNANTS; NEBULA AB Observations with the Hubble Space Telescope (HST), conducted since 1990, now offer an unprecedented glimpse into fast astrophysical shocks in the young remnant of supernova 1987A. Comparing observations taken in 2010 with the use of the refurbished instruments on HST with data taken in 2004, just before the Space Telescope Imaging Spectrograph failed, we find that the Ly alpha and H alpha lines from shock emission continue to brighten, whereas their maximum velocities continue to decrease. We observe broad, blueshifted Ly alpha, which we attribute to resonant scattering of photons emitted from hot spots on the equatorial ring. We also detect N v lambda lambda 1239, 1243 angstrom line emission, but only to the red of Ly alpha. The profiles of the N v lines differ markedly from that of H alpha, suggesting that the N(4+) ions are scattered and accelerated by turbulent electromagnetic fields that isotropize the ions in the collisionless shock. C1 [Heng, Kevin] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [France, Kevin; Stocke, John T.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [McCray, Richard] Univ Colorado, JILA, Boulder, CO 80309 USA. [Heng, Kevin] Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA. [Kirshner, Robert P.; Challis, Peter] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bouchet, Patrice] Commissariat Energie Atom & Energies Alternat, Serv Astrophys, FR-91191 Gif Sur Yvette, France. [Crotts, Arlin] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Dwek, Eli; Sonneborn, George] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fransson, Claes; Larsson, Josefin; Sollerman, Jesper] Stockholm Univ, Oskar Klein Ctr, Dept Astron, S-10691 Stockholm, Sweden. [Garnavich, Peter M.] Univ Notre Dame, Notre Dame, IN 46556 USA. [Lawrence, Stephen S.] Hofstra Univ, Dept Phys & Astron, Hempstead, NY 11549 USA. [Panagia, Nino] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Panagia, Nino] Osserv Astrofis Catania, Inst Nazl Astrofis, I-95123 Catania, Italy. [Pun, Chun S. J.] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Smith, Nathan] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Wang, Lifan] Texas A&M Univ, Dept Phys & Astron, College Stn, TX USA. [Wheeler, J. Craig] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Heng, K (reprint author), ETH, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. EM kheng@phys.ethz.ch RI Dwek, Eli/C-3995-2012; Sonneborn, George/D-5255-2012; OI Sollerman, Jesper/0000-0003-1546-6615; /0000-0003-0065-2933 FU Space Telescope Science Institute [GO-11181]; NASA [NAS5-26555] FX K.F. thanks M. Beasley for enjoyable discussions. Support for this research was provided by NASA through grant GO-11181 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, under NASA contract NAS5-26555. NR 25 TC 12 Z9 12 U1 0 U2 12 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD SEP 24 PY 2010 VL 329 IS 5999 BP 1624 EP 1627 DI 10.1126/science.1192134 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 653NK UT WOS:000282098100034 PM 20813921 ER PT J AU Johnson, WE Onorato, DP Roelke, ME Land, ED Cunningham, M Belden, RC McBride, R Jansen, D Lotz, M Shindle, D Howard, J Wildt, DE Penfold, LM Hostetler, JA Oli, MK O'Brien, SJ AF Johnson, Warren E. Onorato, David P. Roelke, Melody E. Land, E. Darrell Cunningham, Mark Belden, Robert C. McBride, Roy Jansen, Deborah Lotz, Mark Shindle, David Howard, JoGayle Wildt, David E. Penfold, Linda M. Hostetler, Jeffrey A. Oli, Madan K. O'Brien, Stephen J. TI Genetic Restoration of the Florida Panther SO SCIENCE LA English DT Article ID FELIS-CONCOLOR-CORYI; CONSERVATION BIOLOGY; DEPLETION; PUMAS AB The rediscovery of remnant Florida panthers (Puma concolor coryi) in southern Florida swamplands prompted a program to protect and stabilize the population. In 1995, conservation managers translocated eight female pumas (P. c. stanleyana) from Texas to increase depleted genetic diversity, improve population numbers, and reverse indications of inbreeding depression. We have assessed the demographic, population-genetic, and biomedical consequences of this restoration experiment and show that panther numbers increased threefold, genetic heterozygosity doubled, survival and fitness measures improved, and inbreeding correlates declined significantly. Although these results are encouraging, continued habitat loss, persistent inbreeding, infectious agents, and possible habitat saturation pose new dilemmas. This intensive management program illustrates the challenges of maintaining populations of large predators worldwide. C1 [Johnson, Warren E.; O'Brien, Stephen J.] NCI, Lab Genom Divers, Frederick, MD 21702 USA. [Onorato, David P.; Land, E. Darrell; Cunningham, Mark; Lotz, Mark; Shindle, David] Florida Fish & Wildlife Conservat Commiss, Naples, FL 34114 USA. [Roelke, Melody E.] NCI, SAIC Frederick, Lab Genom Divers, Frederick, MD 21702 USA. [Belden, Robert C.] US Fish & Wildlife Serv, Vero Beach, FL 32960 USA. [McBride, Roy] Livestock Protect Co, Alpine, TX 79832 USA. [Jansen, Deborah] Big Cypress Natl Preserve, Ochopee, FL 34141 USA. [Howard, JoGayle; Wildt, David E.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Penfold, Linda M.] White Oak Conservat Ctr, Yulee, FL 32046 USA. [Hostetler, Jeffrey A.; Oli, Madan K.] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32611 USA. RP Johnson, WE (reprint author), NCI, Lab Genom Divers, Frederick, MD 21702 USA. EM warjohns@mail.nih.gov; Dave.Onorato@MyFWC.com; stephenobrien@nih.gov RI Hostetler, Jeffrey/A-3345-2011; Johnson, Warren/D-4149-2016 OI Hostetler, Jeffrey/0000-0003-3669-1758; Johnson, Warren/0000-0002-5954-186X FU Florida Fish and Wildlife Conservation Commission (FWC); Everglades National Park (EVER); BCNP; U.S. Fish and Wildlife Service; National Cancer Institute, National Institutes of Health (NIH) [N01-CO-12400]; NIH, National Cancer Institute, Center for Cancer Research; Florida Panther Research and Management Trust FX We dedicate this study to the memory of Ulysses Seal and Ernst Mayr, important heroes in the conservation struggle of the Florida panther. Funded by the Florida Fish and Wildlife Conservation Commission (FWC) via purchases of Florida panther license plates. Other major funding for the field work was provided by Everglades National Park (EVER), the BCNP, and federal funds from the U.S. Fish and Wildlife Service (especially in the early years) as well as from the National Cancer Institute, National Institutes of Health (NIH), under contract number N01-CO-12400. This research was supported in part by the Intramural Research Program of NIH, National Cancer Institute, Center for Cancer Research, and the Florida Panther Research and Management Trust Fund. All panther captures, sampling, and radio collaring were authorized by U. S. Fish and Wildlife Service Endangered Species Permits TE01553-3 (FWC) and TE146761-1 (BCNP). We thank many individuals for their help in this project, who are named in SOM reference S25. NR 22 TC 136 Z9 139 U1 34 U2 282 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD SEP 24 PY 2010 VL 329 IS 5999 BP 1641 EP 1645 DI 10.1126/science.1192891 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 653NK UT WOS:000282098100040 PM 20929847 ER PT J AU Robinson, H Skvarla, JJ AF Robinson, Harold Skvarla, John J. TI The restoration of the genus Vernonella Sond. (Vernonieae: Asteraceae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID POLLEN MORPHOLOGY; COMPOSITAE; WORLD AB Vernonella Sond. is restored as a distinct genus from synonymy under Vernonia and Centrapalus. Included are the type species Vernonella africana and 10 additional species with thinly scarious-margined involucral bracts and distinctive small, short-colpate type A pollen. C1 [Robinson, Harold] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. [Skvarla, John J.] Univ Oklahoma, Oklahoma Biol Survey, Dept Bot & Microbiol, Norman, OK 73018 USA. RP Robinson, H (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC 166,POB 37012, Washington, DC 20013 USA. EM robinsoh@si.edu; jskvarla@ou.edu NR 28 TC 4 Z9 5 U1 0 U2 3 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD SEP 23 PY 2010 VL 123 IS 3 BP 181 EP 192 PG 12 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 660UW UT WOS:000282672900001 ER PT J AU Opresko, DM Breedy, O AF Opresko, D. M. Breedy, Odalisca TI A new species of antipatharian coral (Cnidaria: Anthozoa: Antipatharia: Schizopathidae) from the Pacific coast of Costa Rica SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB A new species of antipatharian coral (Anthozoa: Antipatharia) is described from the Pacific coast of Costa Rica. Lillipathes ritamariae, new species, forms large, multi-branched, flabellate colonies that reach a height of 60 cm or more. The genus Lillipathes is characterized by pinnules in four rows and arranged in bilateral alternating pairs. In L. ritamariae, the pinnules occur in only two rows in portions of the corallum; however, the characteristic Lillipathes pinnulation pattern is common enough to support assigning this species to this genus. The species can be distinguished from its cogeners by its very short pinnules (mostly 1-1.5 cm in length) and the development of many of the lateral pinnules into pinnulated branches. In contrast, in L. wingi, the pinnules are up to 5 cm long and only a few in the colony develop into branches. In L. quadribrachiata, the pinnules are up to about 3 cm long, and in Lillipathes lilliei, the pinnules are more than 10 cm in length, and only a small number develop into branches. C1 [Opresko, D. M.] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA. [Breedy, Odalisca] Smithsonian Trop Res Inst, Balboa, Panama. [Breedy, Odalisca] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol, San Jose, Costa Rica. [Breedy, Odalisca] Univ Costa Rica, Ctr Invest Estruct Microscopicas, San Jose, Costa Rica. RP Opresko, DM (reprint author), Oak Ridge Natl Lab, Div Environm Sci, POB 2008, Oak Ridge, TN 37831 USA. EM opreskodm@ornl.gov; odalisca.breedy@ucr.ac.cr FU NSF [OCE-0939557]; Smithsonian Institution; Oak Ridge National Laboratory, Oak Ridge, Tennessee FX The first author is especially grateful to Jorge Cortes for his invitation to visit San Jose to study the antipatharian corals in the university collection and for his kind hospitality during that visit. The authors also wish to thank Rita M. Vargas (Museo de Zoologia, University of Costa Rica) for her assistance with the coral collection. Special thanks to Lisa Levin (Chief Scientist), Greg Rouse and Harim Cha (Scripps Institution of Oceanography, University of California at San Diego) for collecting the material and for providing associated information on the specimens and photographs of the colonies in situ and after collection. The specimens were collected as part of research activities conducted under NSF grant OCE-0939557 to Lisa Levin and Greg Rouse. Photomicrographs were prepared in the Scanning Electron Microscopy Laboratories at the CIEMIC, Microscopic Structures Research Centre, University of Costa Rica, San Jose. Thanks also to C. Bright, W. Keel, P. Greenhall, and L. Ward of the National Museum of Natural History, Smithsonian Institution for their assistance during the first author's visit to the Museum Support Center and for processing the type material. The authors appreciate the indepth reviews of the manuscript by T. Molodtsova and a second anonymous reviewer.; This work was supported in part by the Smithsonian Institution; and Oak Ridge National Laboratory, Oak Ridge, Tennessee. D. Opresko is a Research Associate at the National Museum of Natural History, Smithsonian Institution, and gratefully acknowledges that affiliation. NR 7 TC 2 Z9 2 U1 0 U2 2 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD SEP 23 PY 2010 VL 123 IS 3 BP 234 EP 241 PG 8 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 660UW UT WOS:000282672900006 ER PT J AU Micheli, CJ AF Micheli, Charyn J. TI Nomenclatural changes within West Indian Acanthocinini (Coleoptera: Cerambycidae: Lamiinae) SO ZOOTAXA LA English DT Letter C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Micheli, CJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, POB 37012,MRC 187, Washington, DC 20013 USA. EM MicheliC@si.edu NR 10 TC 0 Z9 0 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD SEP 23 PY 2010 IS 2622 BP 65 EP 67 PG 3 WC Zoology SC Zoology GA 657VC UT WOS:000282444900005 ER PT J AU Chen, GX Kirby, K Brickhouse, NS Lin, T Silver, E AF Chen, G. X. Kirby, K. Brickhouse, N. S. Lin, T. Silver, E. TI Reply to "Comment on 'Dirac R-matrix method for the calculation of x-ray line polarization'" SO PHYSICAL REVIEW A LA English DT Letter AB In response to the Comment written by Zhang et al. [Phys. Rev. A 82, 036701 (2010)] we show that the main ideas and results (about the physics and method) reported in our paper [Phys. Rev. A 79, 062715 (2009)] still appear to be correct. Although none of the conjectures given in the Comment about the potential problems in our code are correct, there was a small error in our code, so the part of our paper with numerical data, presented to support our method, appears to be incorrect. The wealth of resonance features in the x-ray line 3D demonstrated in our paper still appears to be real and is reconfirmed by a revised calculation with the error fixed. C1 [Chen, G. X.; Kirby, K.; Brickhouse, N. S.; Lin, T.; Silver, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chen, GX (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Brickhouse, Nancy/0000-0002-8704-4473 NR 5 TC 3 Z9 3 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD SEP 22 PY 2010 VL 82 IS 3 AR 036702 DI 10.1103/PhysRevA.82.036702 PG 2 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 653ML UT WOS:000282095500014 ER PT J AU Vari, RP Zanata, AM Camelier, P AF Vari, Richard P. Zanata, Angela M. Camelier, Priscila TI New Species of Cyphocharax (Ostariophysi: Characiformes: Curimatidae) from the Rio de Contas Drainage, Bahia, Brazil SO COPEIA LA English DT Article AB Cyphocharax pinnilepis, a species of curimatid characiform apparently endemic to the Rio de Contas system in Bahia, Brazil, is described as new. It is only the sixth member of the Curimatidae known from the coastal rivers of Brazil across the expanse from south of the mouth of the Amazon River to the state of Sao Paulo, but the third curimatid species from the Rio de Contas. The basis for the assignment of the species to Cyphocharax is discussed, and it is diagnosed from congeners on details of pigmentation, the pattern of scales on the lobes of the caudal fin, meristics, and morphometrics. C1 [Vari, Richard P.] Smithsonian Inst, Div Fishes, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. [Zanata, Angela M.; Camelier, Priscila] Univ Fed Bahia, Dept Zool, Inst Biol, BR-40170290 Salvador, BA, Brazil. RP Vari, RP (reprint author), Smithsonian Inst, Div Fishes, Dept Vertebrate Zool, Natl Museum Nat Hist, MRC-159,POB 37012, Washington, DC 20013 USA. EM varir@si.edu; a_zanata@yahoo.com.br; pricamelier@yahoo.com.br FU Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology in the Division of Fishes; National Museum of Natural History of the Smithsonian Institution; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico FX Support for this project was provided by the Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology in the Division of Fishes, National Museum of Natural History of the Smithsonian Institution (RPV) and Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (AMZ). E. Baena (MZUSP) assisted with the photography of the holotype, S. Raredon (USNM) with radiography of portions of the type series, and L. Sousa (MZUSP) with the map. R. Burger, A. Goes, and T. Carvalho (all UFBA) participated in the fieldwork that yielded the samples that served as the basis for this paper. P. Carvalho (MZUSP) collected and made available a portion of the paratype series. We thank O. Oyakawa (MZUSP) for the loan of comparative specimens. NR 13 TC 11 Z9 11 U1 0 U2 5 PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS PI MIAMI PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200 SW 8TH STREET, MIAMI, FL 33199 USA SN 0045-8511 EI 1938-5110 J9 COPEIA JI Copeia PD SEP 21 PY 2010 IS 3 BP 382 EP 387 DI 10.1643/CI-09-140 PG 6 WC Zoology SC Zoology GA 655PL UT WOS:000282261800004 ER PT J AU Reece, JS Smith, DG Holm, E AF Reece, Joshua S. Smith, David G. Holm, Erling TI The Moray Eels of the Anarchias cantonensis Group (Anguilliformes: Muraenidae), with Description of Two New Species SO COPEIA LA English DT Article ID HAWAIIAN-ISLANDS; LINE ISLANDS; K-AR; PACIFIC-OCEAN; INDIAN-OCEAN; EVOLUTION; GEOLOGY; AGE; PHILIPPINES; VOLCANISM AB The broadly distributed Indo-Pacific moray eel Anarchlas cantonensis (Schultz, 1943), heretofore treated as a single species, consists of three species: A. cantonensis, A. exulatus, a new species, and A. schultzi, a new species, based on geographic distribution, coloration, external morphometrics, and vertebral counts. We examined 112 specimens and determined that the true A. cantonensis is distributed throughout the eastern Indian Ocean, western Pacific, and tropical central Pacific, and has a mean vertebral formula of 91/93/104. Anarchlas exulatus is distributed anti-tropically in the central and southeastern Pacific and is characterized by a unique mottling pattern and a mean vertebral formula of 100/103/114. A third species, named here as A. schultzi, is characterized by a mean vertebral formula of 96/99/109, a plain brown coloration in adult form, and is restricted geographically to Tonga, New Caledonia, the Solomon Islands, and the Caroline Islands. At the Tonga Islands, which reside on the edge of Australian and Pacific tectonic plates, all three species are present, but maintain their morphological distinctiveness and segregate ecologically. C1 [Reece, Joshua S.] Washington Univ, Dept Biol, St Louis, MO 63130 USA. [Smith, David G.] Museum Support Ctr MRC 534, Div Fishes, Smithsonian Inst, Suitland, MA 20746 USA. [Holm, Erling] Royal Ontario Museum, Dept Nat Hist, Toronto, ON M5S 2C6, Canada. RP Reece, JS (reprint author), Washington Univ, Dept Biol, Box 1137,1 Brookings Dr, St Louis, MO 63130 USA. EM jsreece@wustl.edu; smithd@si.edu; erlingh@rom.on.ca FU Society of Systematic Biologists; DeepFin Fish Phylogeny Project; Smithsonian Institution; Washington University in Saint Louis; AMS; ANSP; BPBM; FMNH; SIO FX Funding for this research was provided by grants to JSR by the Society of Systematic Biologists Mini-PEET Award and the DeepFin Fish Phylogeny Project. Institutional support was provided by the Smithsonian Institution and Washington University in Saint Louis. We thank the following for loan of specimens: M. McGrouther (AMS), M. Sabaj-Perez (ANSP), A. Suzumoto (BPBM), M. Rogers (FMNH), H. Walker (SIO). NR 37 TC 5 Z9 7 U1 0 U2 7 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS PI CHARLESTON PA UNIV CHARLESTON, GRICE MARINE LABORATORY, 205 FORT JOHNSON RD, CHARLESTON, SC 29412 USA SN 0045-8511 J9 COPEIA JI Copeia PD SEP 21 PY 2010 IS 3 BP 421 EP 430 DI 10.1643/CI-09-189 PG 10 WC Zoology SC Zoology GA 655PL UT WOS:000282261800009 ER PT J AU Narayanan, D Dey, A Hayward, CC Cox, TJ Bussmann, RS Brodwin, M Jonsson, P Hopkins, PF Groves, B Younger, JD Hernquist, L AF Narayanan, Desika Dey, Arjun Hayward, Christopher C. Cox, Thomas J. Bussmann, R. Shane Brodwin, Mark Jonsson, Patrik Hopkins, Philip F. Groves, Brent Younger, Joshua D. Hernquist, Lars TI A physical model for z similar to 2 dust-obscured galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE dust, extinction; galaxies: formation; galaxies: high-redshift; galaxies: ISM; galaxies: starburst; cosmology: theory ID ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES; ULTRALUMINOUS INFRARED GALAXIES; SPECTRAL ENERGY-DISTRIBUTION; REDSHIFT SUBMILLIMETER GALAXIES; SUPERMASSIVE BLACK-HOLES; PARTICLE HYDRODYNAMICS SIMULATIONS; SPITZER MIDINFRARED SPECTROSCOPY; POLYCYCLIC AROMATIC-HYDROCARBON; STELLAR MASS DENSITY AB We present a physical model for the origin of z similar to 2 dust-obscured galaxies (DOGs), a class of high-redshift ultraluminous infrared galaxies (ULIRGs) selected at 24 mu m which are particularly optically faint (F(24 mu m)/F(R) > 1000). By combining N-body/smoothed particle hydrodynamic simulations of high-redshift galaxy evolution with 3D polychromatic dust radiative transfer models, we find that luminous DOGs (with F(24) greater than or similar to 0.3mJy at z similar to 2) are well modelled as extreme gas-rich mergers in massive (similar to 5 x 10(12)-10(13) M(circle dot)) haloes, with elevated star formation rates (SFR; similar to 500-1000M(circle dot)yr(-1)) and/or significant active galactic nuclei (AGN) growth (M BH greater than or similar to 0.5M(circle dot) yr(-1)), whereas less luminous DOGs are more diverse in nature. At final coalescence, merger-driven DOGs transition from being starburst dominated to AGN dominated, evolving from a 'bump' to a power-law (PL) shaped mid-IR (Infrared Array Camera, IRAC) spectral energy distribution (SED). After the DOG phase, the galaxy settles back to exhibiting a 'bump' SED with bluer colours and lower SFRs. While canonically PL galaxies are associated with being AGN dominated, we find that the PL mid-IR SED can owe both to direct AGN contribution and to a heavily dust obscured stellar bump at times that the galaxy is starburst dominated. Thus, PL galaxies can be either starburst or AGN dominated. Less luminous DOGs can be well-represented either by mergers or by massive (M(baryon) similar to 5 x 10(11)M(circle dot)) secularly evolving gas-rich disc galaxies (with SFR similar to 50M(circle dot) yr(-1)). By utilizing similar models as those employed in the submillimetre galaxy (SMG) formation study of Narayanan et al., we investigate the connection between DOGs and SMGs. We find that the most heavily star-forming merger-driven DOGs can be selected as submillimetre galaxies, while both merger-driven and secularly evolving DOGs typically satisfy the BzK selection criteria. The model SEDs from the simulated galaxies match observed data reasonably well, though Mrk 231 and Arp 220 templates provide worse matches. Our models provide testable predictions of the physical masses, dust temperatures, CO linewidths and location on the MBH-Mbulge relation of DOGs. Finally, we provide public SED templates derived from these simulations. C1 [Narayanan, Desika; Hayward, Christopher C.; Cox, Thomas J.; Brodwin, Mark; Younger, Joshua D.; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dey, Arjun] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Cox, Thomas J.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Bussmann, R. Shane] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Jonsson, Patrik] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Hopkins, Philip F.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Hopkins, Philip F.] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA. [Groves, Brent] Leiden Univ, Sterrewacht Leiden, NL-233 CA Leiden, Netherlands. [Younger, Joshua D.] Inst Adv Study, Princeton, NJ 08544 USA. RP Narayanan, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dnarayanan@cfa.harvard.edu RI Hayward, Christopher/I-4756-2012 OI Hayward, Christopher/0000-0003-4073-3236 FU W. M. Keck Foundation [GO10890]; AURA [NAS5-26555, HST-AR-10678, 10958] FX We are grateful to Ranga-Ram Chary, Vandana Desai, Brandon Kelly, Kai Noeske, Jason Melbourne and Alex Pope for helpful conversations. DN thanks the NOAO in Tucson for hospitality, where part of this study was conducted. The authors are grateful to the W. M. Keck Foundation for hosting the Napa Galaxy Evolution workshop where the ideas for much of this project came about. AD is supported byNOAO, which is operated by the Association ofUniversities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. CCH was funded by an NSF Graduate Research Fellowship. TC and MB acknowledge support from the W. M. Keck Foundation. RSB acknowledges financial assistance from HST grant GO10890, which is provided by NASA through a grant from the Space Telescope Science Institute which is operated by AURA under NASA contract NAS5-26555. PJ was supported by programsHST-AR-10678 and 10958, provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555, and by Spitzer Theory Grant 30183 from the Jet Propulsion Laboratory. Support for PFH was provided by the Miller Institute for Basic Research in Science, University of California, Berkeley. The simulations in this paper were run on the Odyssey cluster supported by the Harvard FAS Research Computing Group. NR 149 TC 77 Z9 77 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 21 PY 2010 VL 407 IS 3 BP 1701 EP 1720 DI 10.1111/j.1365-2966.2010.16997.x PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 649TX UT WOS:000281797900022 ER PT J AU Bloemen, S Marsh, TR Steeghs, D Ostensen, RH AF Bloemen, S. Marsh, T. R. Steeghs, D. Ostensen, R. H. TI Spin-resolved spectroscopy of the intermediate polar DQ Her SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; binaries: close; binaries: eclipsing; stars: individual: DQ Herculis; novae, cataclysmic variables ID RAPID LIGHT VARIATIONS; 71 2ND OSCILLATION; OLD NOVA DQ; ACCRETION DISKS; CATACLYSMIC VARIABLES; HERCULIS 1934; DOPPLER TOMOGRAPHY; SPIRAL STRUCTURE; BINARY-SYSTEMS; SPACED DATA AB We present high-speed spectroscopic observations of the intermediate polar (IP) DQ Herculis. Doppler tomography of two He I lines reveals a spiral density structure in the accretion disc around the white dwarf (WD) primary. The spirals look very similar to the spirals seen in dwarf novae during outburst. DQ Her is the first well-established IP in which spirals are seen, which are in addition likely persistent because of the system's high mass transfer rate. Spiral structures give an alternative explanation for sidebands of the WD spin frequency that are found in IP light curves. The Doppler tomogram of He II lambda 4686 indicates that a large part of the emission is not disc-like. Spin trails of spectra reveal a pulsation in the He II lambda 4686 emission that is believed to result from reprocessing of X-rays from the WD's magnetic poles in the accretion flow close to the WD. We confirm the previous finding that the pulsation is only visible in the redshifted part of the line when the beam points to the back side of the disc. The absence of reprocessed light from the front side of the disc can be explained by obscuration by the front rim of the disc, but the absence of extra emission from the blueshifted back side of the disc is puzzling. Reprocessing in accretion curtains can be an answer to the problem and can also explain the highly non-Keplerian velocity components that are found in the He II lambda 4686 line. Our spin trails can form a strong test for future accretion curtain models, with the possibility of distinguishing between a spin period of 71 or 142 s. Spin trails of data taken at selected orbital phases show little evidence for a significant contribution of the bright spot to the pulsations and allow us to exclude a recent suggestion that 71 s is the beat period and 70.8 s the spin period. C1 [Bloemen, S.; Ostensen, R. H.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Leuven, Belgium. [Marsh, T. R.; Steeghs, D.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Steeghs, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bloemen, S (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Leuven, Belgium. EM steven.bloemen@ster.kuleuven.be RI Steeghs, Danny/C-5468-2009 OI Steeghs, Danny/0000-0003-0771-4746 FU European Research Council under the European Community [227224]; Research Council of K. U. Leuven [GOA/2008/04]; UK's Science and Technology Facilities Council (STFC) [ST/F002599/1, PP/D005914/1] FX The research leading to these results has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 227224 (PROSPERITY), as well as from the Research Council of K. U. Leuven grant agreement GOA/2008/04. During this research TRM and DS were supported under grants from the UK's Science and Technology Facilities Council (STFC; ST/F002599/1 and PP/D005914/1). NR 49 TC 8 Z9 8 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 21 PY 2010 VL 407 IS 3 BP 1903 EP 1912 DI 10.1111/j.1365-2966.2010.17035.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 649TX UT WOS:000281797900040 ER PT J AU Chen, HX Strand, M Norenburg, JL Sun, SC Kajihara, H Chernyshev, AV Maslakova, SA Sundberg, P AF Chen, Haixia Strand, Malin Norenburg, Jon L. Sun, Shichun Kajihara, Hiroshi Chernyshev, Alexey V. Maslakova, Svetlana A. Sundberg, Per TI Statistical Parsimony Networks and Species Assemblages in Cephalotrichid Nemerteans (Nemertea) SO PLOS ONE LA English DT Article ID PHYLUM NEMERTEA; DNA TAXONOMY; SEQUENCES; ARCHINEMERTEA; DELIMITATION; PHYLOGENY; INTERFACE; CHECKLIST; ANOPLA; GENERA AB Background: It has been suggested that statistical parsimony network analysis could be used to get an indication of species represented in a set of nucleotide data, and the approach has been used to discuss species boundaries in some taxa. Methodology/Principal Findings: Based on 635 base pairs of the mitochondrial protein-coding gene cytochrome c oxidase I (COI), we analyzed 152 nemertean specimens using statistical parsimony network analysis with the connection probability set to 95%. The analysis revealed 15 distinct networks together with seven singletons. Statistical parsimony yielded three networks supporting the species status of Cephalothrix rufifrons, C. major and C. spiralis as they currently have been delineated by morphological characters and geographical location. Many other networks contained haplotypes from nearby geographical locations. Cladistic structure by maximum likelihood analysis overall supported the network analysis, but indicated a false positive result where subnetworks should have been connected into one network/species. This probably is caused by undersampling of the intraspecific haplotype diversity. Conclusions/Significance: Statistical parsimony network analysis provides a rapid and useful tool for detecting possible undescribed/cryptic species among cephalotrichid nemerteans based on COI gene. It should be combined with phylogenetic analysis to get indications of false positive results, i.e., subnetworks that would have been connected with more extensive haplotype sampling. C1 [Chen, Haixia; Sun, Shichun] Ocean Univ China, Inst Evolut & Marine Biodivers, Qingdao, Peoples R China. [Chen, Haixia; Sundberg, Per] Univ Gothenburg, Dept Zool, Gothenburg, Sweden. [Strand, Malin] Sven Loven Ctr Marine Sci, Tjarno, Sweden. [Norenburg, Jon L.] Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. [Kajihara, Hiroshi] Hokkaido Univ, Fac Sci, Dept Nat Hist Sci, Sapporo, Hokkaido 060, Japan. [Chernyshev, Alexey V.] Russian Acad Sci, Far E Div, AV Zhirmunsky Inst Marine Biol, Vladivostok 690022, Russia. [Maslakova, Svetlana A.] Univ Oregon, Oregon Inst Marine Biol, Charleston, OR USA. RP Chen, HX (reprint author), Ocean Univ China, Inst Evolut & Marine Biodivers, Qingdao, Peoples R China. EM p.sundberg@zool.gu.se RI Kajihara, Hiroshi/A-8822-2012; Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 FU National Natural Science Foundation of China [30970333]; Swedish Research Council; Research Institute of Marine Invertebrates, Japan [FY2008]; NSF [DEB 9712463]; Smithsonian Institution FX The study was supported by the National Natural Science Foundation of China (30970333 to SCS), the Swedish Research Council (to PS), the Research Institute of Marine Invertebrates, Japan (FY2008, No. 14 to HK), NSF PEET award (DEB 9712463 to JLN) and various funds from the Smithsonian Institution. This publication represents contribution 817 of the Smithsonian Marine Station at Fort Pierce, Florida and 891 of the Smithsonian Caribbean Coral Reef Ecosystem program in Belize. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 43 TC 35 Z9 37 U1 0 U2 9 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD SEP 21 PY 2010 VL 5 IS 9 AR e12885 DI 10.1371/journal.pone.0012885 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 652JO UT WOS:000282002900017 PM 20877627 ER PT J AU Greene, JE Peng, CY Kim, MJ Kuo, CY Braatz, JA Impellizzeri, CMV Condon, JJ Lo, KY Henkel, C Reid, MJ AF Greene, Jenny E. Peng, Chien Y. Kim, Minjin Kuo, Cheng-Yu Braatz, James A. Impellizzeri, C. M. Violette Condon, James J. Lo, K. Y. Henkel, Christian Reid, Mark J. TI PRECISE BLACK HOLE MASSES FROM MEGAMASER DISKS: BLACK HOLE-BULGE RELATIONS AT LOW MASS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: bulges; galaxies: nuclei; galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; EARLY-TYPE GALAXIES; DIGITAL SKY SURVEY; AGN MONITORING PROJECT; LATE-TYPE SPIRALS; VELOCITY DISPERSION CORRELATION; DWARF SEYFERT NUCLEI; BROAD-LINE REGION; BH-SIGMA RELATION; ACCRETION DISK AB The black hole (BH)-bulge correlations have greatly influenced the last decade of efforts to understand galaxy evolution. Current knowledge of these correlations is limited predominantly to high BH masses (M(BH) greater than or similar to 10(8) M(circle dot)) that can be measured using direct stellar, gas, and maser kinematics. These objects, however, do not represent the demographics of more typical L < L* galaxies. This study transcends prior limitations to probe BHs that are an order of magnitude lower in mass, using BH mass measurements derived from the dynamics of H(2)O megamasers in circumnuclear disks. The masers trace the Keplerian rotation of circumnuclear molecular disks starting at radii of a few tenths of a pc from the central BH. Modeling of the rotation curves, presented by Kuo et al., yields BH masses with exquisite precision. We present stellar velocity dispersion measurements for a sample of nine megamaser disk galaxies based on long-slit observations using the B&C spectrograph on the Dupont telescope and the Dual Imaging Spectrograph on the 3.5 m telescope at Apache Point. We also perform bulge-to-disk decomposition of a subset of five of these galaxies with Sloan Digital Sky Survey imaging. The maser galaxies as a group fall below the M(BH)-sigma(*) relation defined by elliptical galaxies. We show, now with very precise BH mass measurements, that the low-scatter power-law relation between M(BH) and sigma(*) seen in elliptical galaxies is not universal. The elliptical galaxy M(BH)-sigma* relation cannot be used to derive the BH mass function at low mass or the zero point for active BH masses. The processes (perhaps BH self-regulation or minor merging) that operate at higher mass have not effectively established an M(BH)-sigma* relation in this low-mass regime. C1 [Greene, Jenny E.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Peng, Chien Y.] NRC Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Kim, Minjin; Kuo, Cheng-Yu; Braatz, James A.; Impellizzeri, C. M. Violette; Condon, James J.; Lo, K. Y.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Henkel, Christian] Max Planck Inst Radio Astron, Bonn, Germany. [Reid, Mark J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Greene, JE (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. FU National Aeronautics and Space Administration; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences; Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington FX Many people have contributed substantively to our thinking in the writing of this paper. We first thank the referee for a very prompt and thorough report. We gratefully acknowledge useful conversations with A. Barth, L. Ho, J. Kormendy, G. van de Venn, and N. Drory. P. Erwin and J. Mulchaey both provided optical images of various galaxies presented here and K. Gultekin assisted in our implementation of his fitting methodology. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We further acknowledge the usage of the HyperLeda database (http://leda.univ-lyon1.fr). Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 172 TC 121 Z9 122 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2010 VL 721 IS 1 BP 26 EP 45 DI 10.1088/0004-637X/721/1/26 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TI UT WOS:000282192900002 ER PT J AU Cohen, O Drake, JJ Kashyap, VL Hussain, GAJ Gombosi, TI AF Cohen, O. Drake, J. J. Kashyap, V. L. Hussain, G. A. J. Gombosi, T. I. TI THE CORONAL STRUCTURE OF AB DORADUS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: activity; stars: coronae; stars: magnetic field ID ANGULAR-MOMENTUM LOSS; X-RAY SPECTROSCOPY; SOLAR-TYPE STARS; MAGNETIC-FIELD; DIFFERENTIAL ROTATION; POLYTROPIC INDEX; STELLAR WINDS; EVOLUTION; MODELS; DOR AB We perform a numerical simulation of the corona of the young, rapidly rotating K0 dwarf AB Doradus using a global magnetohydrodynamic (MHD) model. The model is driven by a surface map of the radial magnetic field constructed using Zeeman-Doppler Imaging. We find that the global structure of the stellar corona is dominated by strong azimuthal tangling of the magnetic field due to the rapid rotation. The MHD solution enables us to calculate realistic Alfven surfaces, and we can therefore estimate the stellar mass loss rate and angular momentum loss rate without making undue theoretical simplifications. We consider three cases, parameterized by the base density of the corona, that span the range of possible solutions for the system. We find that overall the mass and angular momentum loss rates are higher than in the solar case; the mass loss rates are 10-500 times higher, and the angular momentum loss rate can be up to 3 x 10(4) higher than present-day solar values. Our simulations show that this model can be used to constrain the wide parameter space of stellar systems. It also shows that an MHD approach can provide more information about the physical system over the commonly used potential field extrapolation. C1 [Cohen, O.; Drake, J. J.; Kashyap, V. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hussain, G. A. J.] ESO, D-85748 Garching, Germany. [Gombosi, T. I.] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA. RP Cohen, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Gombosi, Tamas/G-4238-2011; OI Gombosi, Tamas/0000-0001-9360-4951; Cohen, Ofer/0000-0003-3721-0215 FU SHINE through NSF [ATM-0823592]; NASA [NNG05GM44G, NAS8-39073]; NSF FX We thank to an unknown referee for his/her useful comments. O.C. is supported by SHINE through NSF ATM-0823592 grant, and by NASA-LWSTRT Grant NNG05GM44G. J.J.D. and V. L. K. were funded by NASA contract NAS8-39073 to the Chandra X-ray Center. Simulation results were obtained using the Space Weather Modeling Framework, developed by the Center for Space Environment Modeling, at the University of Michigan with funding support from NASA ESS, NASA ESTO-CT, NSF KDI, and DoD MURI. NR 57 TC 19 Z9 19 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2010 VL 721 IS 1 BP 80 EP 89 DI 10.1088/0004-637X/721/1/80 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TI UT WOS:000282192900006 ER PT J AU Brodwin, M Ruel, J Ade, PAR Aird, KA Andersson, K Ashby, MLN Bautz, M Bazin, G Benson, BA Bleem, LE Carlstrom, JE Chang, CL Crawford, TM Crites, AT De Haan, T Desai, S Dobbs, MA Dudley, JP Fazio, GG Foley, RJ Forman, WR Garmire, G George, EM Gladders, MD Gonzalez, AH Halverson, NW High, FW Holder, GP Holzapfel, WL Hrubes, JD Jones, C Joy, M Keisler, R Knox, L Lee, AT Leitch, EM Lueker, M Marrone, DP McMahon, JJ Mehl, J Meyer, SS Mohr, JJ Montroy, TE Murray, SS Padin, S Plagge, T Pryke, C Reichardt, CL Rest, A Ruhl, JE Schaffer, KK Shaw, L Shirokoff, E Song, J Spieler, HG Stalder, B Stanford, SA Staniszewski, Z Stark, AA Stubbs, CW Vanderlinde, K Vieira, JD Vikhlinin, A Williamson, R Yang, Y Zahn, O Zenteno, A AF Brodwin, M. Ruel, J. Ade, P. A. R. Aird, K. A. Andersson, K. Ashby, M. L. N. Bautz, M. Bazin, G. Benson, B. A. Bleem, L. E. Carlstrom, J. E. Chang, C. L. Crawford, T. M. Crites, A. T. De Haan, T. Desai, S. Dobbs, M. A. Dudley, J. P. Fazio, G. G. Foley, R. J. Forman, W. R. Garmire, G. George, E. M. Gladders, M. D. Gonzalez, A. H. Halverson, N. W. High, F. W. Holder, G. P. Holzapfel, W. L. Hrubes, J. D. Jones, C. Joy, M. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Lueker, M. Marrone, D. P. McMahon, J. J. Mehl, J. Meyer, S. S. Mohr, J. J. Montroy, T. E. Murray, S. S. Padin, S. Plagge, T. Pryke, C. Reichardt, C. L. Rest, A. Ruhl, J. E. Schaffer, K. K. Shaw, L. Shirokoff, E. Song, J. Spieler, H. G. Stalder, B. Stanford, S. A. Staniszewski, Z. Stark, A. A. Stubbs, C. W. Vanderlinde, K. Vieira, J. D. Vikhlinin, A. Williamson, R. Yang, Y. Zahn, O. Zenteno, A. TI SPT-CL J0546-5345: A MASSIVE z > 1 GALAXY CLUSTER SELECTED VIA THE SUNYAEV-ZEL'DOVICH EFFECT WITH THE SOUTH POLE TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (SPT-CL J0546-5345); galaxies: distances and redshifts; galaxies: evolution ID IRAC SHALLOW SURVEY; X-RAY; VELOCITY DISPERSIONS; PHOTOMETRIC REDSHIFTS; TEMPERATURE RELATION; COSMOLOGY; CHANDRA; PROFILES; SAMPLE; GAS AB We report the spectroscopic confirmation of SPT-CL J0546-5345 at < z > = 1.067. To date this is the most distant cluster to be spectroscopically confirmed from the 2008 South Pole Telescope (SPT) catalog, and indeed the first z > 1 cluster discovered by the Sunyaev-Zel'dovich Effect (SZE). We identify 21 secure spectroscopic members within 0.9 Mpc of the SPT cluster position, 18 of which are quiescent, early-type galaxies. From these quiescent galaxies we obtain a velocity dispersion of 1179-(+232)(167) km s(-1), ranking SPT-CL J0546-5345 as the most dynamically massive cluster yet discovered at z > 1. Assuming that SPT-CL J0546-5345 is virialized, this implies a dynamical mass of M(200) = 1.0(-0.4)(+0.6) x 10(15) M(circle dot), in agreement with the X-ray and SZE mass measurements. Combining masses from several independent measures leads to a best-estimate mass of M(200) = (7.95 +/- 0.92) x 10(14) M(circle dot). The spectroscopic confirmation of SPT-CL J0546-5345, discovered in the wide-angle, mass-selected SPT cluster survey, marks the onset of the high-redshift SZE-selected galaxy cluster era. C1 [Brodwin, M.; Ashby, M. L. N.; Fazio, G. G.; Foley, R. J.; Forman, W. R.; Jones, C.; Murray, S. S.; Stalder, B.; Stark, A. A.; Stubbs, C. W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ruel, J.; High, F. W.; Rest, A.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Ade, P. A. R.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. [Aird, K. A.; Hrubes, J. D.; Marrone, D. P.] Univ Chicago, Chicago, IL 60637 USA. [Andersson, K.; Bautz, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Bazin, G.; Mohr, J. J.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Bazin, G.; Mohr, J. J.; Zenteno, A.] Excellence Cluster Univ, D-85758 Garching, Germany. [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Keisler, R.; Leitch, E. M.; Marrone, D. P.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Padin, S.; Pryke, C.; Schaffer, K. K.; Vieira, J. D.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; McMahon, J. J.; Meyer, S. S.; Pryke, C.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [De Haan, T.; Dobbs, M. A.; Dudley, J. P.; Holder, G. P.; Shaw, L.; Vanderlinde, K.] McGill Univ, Dept Phys, Quebec City, PQ H3A 2T8, Canada. [Desai, S.; Song, J.; Yang, Y.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Garmire, G.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [George, E. M.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Plagge, T.; Reichardt, C. L.; Shirokoff, E.; Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Joy, M.] NASA Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. [Knox, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Phys, Berkeley, CA 94720 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Cleveland, OH 44106 USA. [Montroy, T. E.; Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, CERCA, Cleveland, OH 44106 USA. [Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. RP Brodwin, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Stubbs, Christopher/C-2829-2012; Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Stark, Antony/0000-0002-2718-9996; Stubbs, Christopher/0000-0003-0347-1724; Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169 FU National Science Foundation [ANT-0638937]; NSF Physics Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; NASA; Chandra Xray Observatory [SV4-74018, A31]; W. M. Keck Foundation; Brinson Foundation FX Visiting astronomer, Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, under contract with the National Science Foundation; The SPT is supported by the National Science Foundation through grant ANT-0638937. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. This paper includes data gathered with the 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile. This work is based in part on observations obtained with the Chandra Xray Observatory, under contract SV4-74018, A31 with the Smithsonian Astrophysical Observatory which operates the Chandra for NASA. We are very grateful for the efforts of the Spitzer, Chandra, Magellan, and CTIO support staff without whom this paper would not be possible. Support for M. B. was provided by the W. M. Keck Foundation. B. S. acknowledges support from the Brinson Foundation. NR 60 TC 74 Z9 75 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2010 VL 721 IS 1 BP 90 EP 97 DI 10.1088/0004-637X/721/1/90 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TI UT WOS:000282192900007 ER PT J AU Kartaltepe, JS Sanders, DB Le Floc'h, E Frayer, DT Aussel, H Arnouts, S Ilbert, O Salvato, M Scoville, NZ Surace, J Yan, L Capak, P Caputi, K Carollo, CM Cassata, P Civano, F Hasinger, G Koekemoer, AM Le Fevre, O Lilly, S Liu, CT McCracken, HJ Schinnerer, E Smolcic, V Taniguchi, Y Thompson, DJ Trump, J Baldassare, VF Fiorenza, SL AF Kartaltepe, Jeyhan S. Sanders, D. B. Le Floc'h, E. Frayer, D. T. Aussel, H. Arnouts, S. Ilbert, O. Salvato, M. Scoville, N. Z. Surace, J. Yan, L. Capak, P. Caputi, K. Carollo, C. M. Cassata, P. Civano, F. Hasinger, G. Koekemoer, A. M. Le Fevre, O. Lilly, S. Liu, C. T. McCracken, H. J. Schinnerer, E. Smolcic, V. Taniguchi, Y. Thompson, D. J. Trump, J. Baldassare, V. F. Fiorenza, S. L. TI A MULTIWAVELENGTH STUDY OF A SAMPLE OF 70 mu m SELECTED GALAXIES IN THE COSMOS FIELD. II. THE ROLE OF MERGERS IN GALAXY EVOLUTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: active; galaxies: evolution; galaxies: high-redshift; infrared: galaxies; surveys ID ACTIVE GALACTIC NUCLEI; ULTRALUMINOUS INFRARED GALAXIES; DUST-OBSCURED GALAXIES; STAR-FORMATION RATES; DIGITAL SKY SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; COLOR-MAGNITUDE RELATION; MEDIUM DEEP SURVEY; LUMINOSITY FUNCTION; REDSHIFT SURVEY AB We analyze the morphological properties of a large sample of 1503 70 mu m selected galaxies in the COSMOS field spanning the redshift range 0.01 < z < 3.5 with a median redshift of 0.5 and an infrared luminosity range of 10(8) < L-IR(8-1000 mu m) < 10(14) L-circle dot with a median luminosity of 10(11.4) L-circle dot. In general, these galaxies are massive, with a stellar mass range of 10(10)-10(12) M-circle dot, and luminous, with -25 < M-K < -20. We find a strong correlation between the fraction of major mergers and L-IR, with the fraction at the highest luminosity (L-IR > 10(12) L-circle dot) being up to similar to 50%. We also find that the fraction of spirals drops dramatically with LIR. Minor mergers likely play a role in boosting the infrared luminosity for sources with low luminosities (L-IR < 10(11.5) L-circle dot). The precise fraction of mergers in any given L-IR bin varies by redshift due to sources at z > 1 being difficult to classify and subject to the effects of bandpass shifting; therefore, these numbers can only be considered lower limits. At z < 1, where the morphological classifications are most robust, major mergers clearly dominate the ULIRG population (similar to 50%-80%) and are important for the LIRG population (similar to 25%-40%). At z > 1, the fraction of major mergers is lower, but is at least 30%-40% for ULIRGs. In a comparison of our visual classifications with several automated classification techniques we find general agreement; however, the fraction of identified mergers is underestimated due to automated classification methods being sensitive to only certain timescales of a major merger. Although the general morphological trends agree with what has been observed for local (U) LIRGs, the fraction of major mergers is slightly lower than seen locally. This is in part due to the difficulty of identifying merger signatures at high redshift. The distribution of the U-V color of the galaxies in our sample peaks in the green valley (< U - V > = 1.1) with a large spread at bluer and redder colors and with the major mergers peaking more strongly in the green valley than the rest of the morphological classes. We argue that, given the number of major gas-rich mergers observed and the relatively short timescale that they would be observable in the (U) LIRG phase, it is plausible for the observed red sequence of massive ellipticals (< 10(12) M-circle dot) to have been formed entirely by gas-rich major mergers. C1 [Kartaltepe, Jeyhan S.; Sanders, D. B.; Le Floc'h, E.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Kartaltepe, Jeyhan S.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Le Floc'h, E.; Aussel, H.] Univ Paris 07, CNRS, AIM Unite Mixte Rech, CEA CNRS,UMR 7158, F-91191 Gif Sur Yvette, France. [Frayer, D. T.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Arnouts, S.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Ilbert, O.; Cassata, P.; Le Fevre, O.] Lab Astrophys Marseille, F-13376 Marseille 12, France. [Salvato, M.; Scoville, N. Z.; Capak, P.; Smolcic, V.] CALTECH, MC 105 24, Pasadena, CA 91125 USA. [Surace, J.; Yan, L.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Caputi, K.; Carollo, C. M.; Lilly, S.] ETH, Dept Phys, CH-8093 Zurich, Switzerland. [Civano, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hasinger, G.] Max Planck Inst Extraterr Phys, D-85478 Garching, Germany. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Liu, C. T.; Fiorenza, S. L.] CUNY, Coll Staten Isl, Astrophys Observ, Staten Isl, NY 10314 USA. [McCracken, H. J.] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France. [Schinnerer, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Taniguchi, Y.] Ehime Univ, Dept Phys, Grad Sch Sci, Matsuyama, Ehime 7908577, Japan. [Thompson, D. J.] Univ Arizona, Large Binocular Telescope Observ, Tucson, AZ 85721 USA. [Trump, J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Baldassare, V. F.] CUNY, Dept Phys & Astron, Hunter Coll, New York, NY 10065 USA. RP Kartaltepe, JS (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM jeyhan@noao.edu RI Le Fevre, Olivier/G-7389-2011; OI Koekemoer, Anton/0000-0002-6610-2048 FU NASA [NAS 5-26555, 1282612, 1298213, 1344920]; European Southern Observatory, Chile [175.A-0839]; CFHT Corporation; CEA/DAPNIA; National Research Council of Canada; Canadian Astronomy Data Centre; Centre National de la Recherche Scientifique de France; TERAPIX; University of Hawaii; City University of New York; NSF [AST-0071048]; National Aeronautics and Space Administration; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA Inc, under NASA contract NAS 5-26555; also based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; the XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; the European Southern Observatory under Large Program 175.A-0839, Chile; the National Radio Astronomy Observatory which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc; the Canada-France-Hawaii Telescope with MegaPrime/MegaCam operated as a joint project by the CFHT Corporation, CEA/DAPNIA, the National Research Council of Canada, the Canadian Astronomy Data Centre, the Centre National de la Recherche Scientifique de France, TERAPIX and the University of Hawaii.; Support for this work was provided in part by NASA through contracts 1282612, 1298213, and 1344920 issued by the Jet Propulsion Laboratory. This work was supported in part by a grant from The City University of New York PSC-CUNY Research Award Program. We would also like to recognize the contributions from all of the members of the COSMOS Team who helped in obtaining and reducing the large amount of multi-wavelength data that are now publicly available through the NASA Infrared Science Archive (IRSA) at http://irsa.ipac.caltech.edu/Missions/cosmos.html. The analysis pipeline used to reduce the DEIMOS data was developed at UC Berkeley with support from NSF grant AST-0071048. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has also made use of data from the Sloan Digital Sky Survey (SDSS-DR7). Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. We thank the anonymous referee for their thorough comments, which greatly improved the paper. We also thank Marco Barden and Knud Jhanke for the use of the FERENGI redshifting code as well as their help with using it. NR 103 TC 78 Z9 78 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2010 VL 721 IS 1 BP 98 EP 123 DI 10.1088/0004-637X/721/1/98 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TI UT WOS:000282192900008 ER PT J AU Romita, KA Carlson, LR Meixner, M Sewilo, M Whitney, B Babler, B Indebetouw, R Hora, JL Meade, M Shiao, B AF Romita, Krista Alexandra Carlson, Lynn Redding Meixner, M. Sewilo, M. Whitney, B. Babler, B. Indebetouw, R. Hora, J. L. Meade, M. Shiao, B. TI YOUNG STELLAR OBJECTS IN THE LARGE MAGELLANIC CLOUD STAR-FORMING REGION N206 SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: stars; ISM: individual objects (N206); Magellanic Clouds; stars: formation; stars: pre-main sequence ID 2-DIMENSIONAL RADIATIVE-TRANSFER; SPECTRAL ENERGY-DISTRIBUTIONS; PROTOSTELLAR ENVELOPES; SUPERNOVA-REMNANTS; SPITZER ANALYSIS; MASSIVE STARS; SAGE; SEQUENCE; 2MASS; EVOLUTION AB We present analysis of the energetic star-forming region Henize 206 (N206) located near the southern edge of the Large Magellanic Cloud (LMC) based on photometric data from the Spitzer Surveying the Agents of Galaxy Evolution (SAGE-LMC; IRAC 3.6, 4.5, 5.8, 8.0 mu m and MIPS 24 mu m), Infrared Survey Facility near-infrared survey (J, H, K(s)), and the Magellanic Clouds Photometric Survey (MCPS UBVI) covering a wavelength range of 0.36-24 mu m. Young stellar object (YSO) candidates are identified based upon their location in infrared color-magnitude space and classified by the shapes of their spectral energy distributions in comparison with a pre-computed grid of YSO models. We identify 116 YSO candidates: 102 are well characterized by the YSO models, predominately Stage I, and 14 may be multiple sources or young sources with transition disks. Careful examination of the individual sources and their surrounding environment allows us to identify a factor of similar to 14.5 more YSO candidates than have already been identified. The total mass of these well-fit YSO candidates is similar to 520 M(circle dot). We calculate a current star formation rate of 0.27 x 10(-1) M(circle dot) yr(-1) kpc(-2). The distribution of YSO candidates appears to follow shells of neutral material in the interstellar medium. C1 [Romita, Krista Alexandra; Meixner, M.; Sewilo, M.; Shiao, B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Carlson, Lynn Redding] Johns Hopkins Univ, Baltimore, MD USA. [Whitney, B.] Space Sci Inst, Boulder, CO USA. [Babler, B.; Meade, M.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Indebetouw, R.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Hora, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Romita, KA (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM k.a.romita@gmail.com; carlson@stsci.edu; bwhitney@spacescience.org; brian@sal.wisc.edu; remy@virginia.edu; jhora@cfa.harvard.edu OI Babler, Brian/0000-0002-6984-5752; Hora, Joseph/0000-0002-5599-4650 NR 41 TC 7 Z9 7 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2010 VL 721 IS 1 BP 357 EP 368 DI 10.1088/0004-637X/721/1/357 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TI UT WOS:000282192900023 ER PT J AU Broderick, AE Keto, E AF Broderick, Avery E. Keto, Eric TI THE EVOLUTION OF CLOUD CORES AND THE FORMATION OF STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; ISM: clouds; ISM: kinematics and dynamics; stars: formation ID PRE-STELLAR CORES; OSCILLATING STARLESS CORES; CARLO RADIATIVE-TRANSFER; INITIAL CONDITIONS; DARK CLOUDS; DENSE CORES; PRESTELLAR CORES; DYNAMICAL STATE; TEMPERATURE; EXTINCTION AB For a number of starless cores, self-absorbed molecular line and column density observations have implied the presence of large-amplitude oscillations. We examine the consequences of these oscillations on the evolution of the cores and the interpretation of their observations. We find that the pulsation energy helps support the cores and that the dissipation of this energy can lead toward instability and star formation. In this picture, the core lifetimes are limited by the pulsation-decay timescales, dominated by non-linear mode-mode coupling, and on the order of similar or equal to few x 10(5)-10(6) yr. Notably, this is similar to what is required to explain the relatively low rate of conversion of cores into stars. For cores with large-amplitude oscillations, dust continuum observations may appear asymmetric or irregular. As a consequence, some of the cores that would be classified as super-critical may be dynamically stable when oscillations are taken into account. Thus, our investigation motivates a simple hydrodynamic picture, capable of reproducing many of the features of the progenitors of stars without the inclusion of additional physical processes, such as large-scale magnetic fields. C1 [Broderick, Avery E.] Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Keto, Eric] Smithsonian Observ, Cambridge, MA 02138 USA. RP Broderick, AE (reprint author), Canadian Inst Theoret Astrophys, 60 St George St, Toronto, ON M5S 3H8, Canada. EM aeb@cita.utoronto.ca; keto@cfa.harvard.edu NR 48 TC 8 Z9 8 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2010 VL 721 IS 1 BP 493 EP 504 DI 10.1088/0004-637X/721/1/493 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TI UT WOS:000282192900033 ER PT J AU Koch, PM Tang, YW Ho, PTP AF Koch, Patrick M. Tang, Ya-Wen Ho, Paul T. P. TI MAGNETIC FIELD PROPERTIES IN HIGH-MASS STAR FORMATION FROM LARGE TO SMALL SCALES: A STATISTICAL ANALYSIS FROM POLARIZATION DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: individual objects (W51 e2/e8, Orion BN/KL); ISM: magnetic fields; methods: statistical; polarization; turbulence ID FAR-INFRARED POLARIMETRY; MOLECULAR CLOUDS; SUBMILLIMETER POLARIZATION; RADIATIVE TORQUES; GRAIN ALIGNMENT; FORMING REGIONS; INTERSTELLAR GRAINS; CORES; ORION; DISPERSION AB Polarization data from high-mass star formation regions (W51 e2/e8, Orion BN/KL) are used to derive statistical properties of the plane of sky projected magnetic field. Structure function and auto-correlation function are calculated for observations with various resolutions from the BIMA and SMA interferometers, covering a range in physical scales from similar to 70 mpc to similar to 2.1 mpc. Results for the magnetic field turbulent dispersion, its turbulent-to-mean field strength ratio, and the large-scale polarization angle correlation length are presented as a function of the physical scale at the star formation sites. Power-law scaling relations emerge for some of these physical quantities. The turbulent-to-mean field strength ratio is found to be close to constant over the sampled observing range, with a hint of a decrease toward smaller scales, indicating that the role of the magnetic field and turbulence is evolving with the physical scale. A statistical method is proposed to separate large-and small-scale correlations from an initial ensemble of polarization segments. This also leads to a definition of a turbulent polarization angle correlation length. C1 [Koch, Patrick M.; Tang, Ya-Wen; Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Koch, PM (reprint author), Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. EM pmkoch@asiaa.sinica.edu.tw OI Tang, Ya-Wen/0000-0002-0675-276X FU NSC [NSC98-2119-M-001-024-MY4] FX The authors thank the referees, Roger H. Hildebrand, Martin Houde, and John E. Vaillancourt for their comments and explanations which provided important further insight. Y.-W.T. and P. T. P. H. are supported by NSC grant NSC98-2119-M-001-024-MY4. NR 48 TC 14 Z9 14 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2010 VL 721 IS 1 BP 815 EP 827 DI 10.1088/0004-637X/721/1/815 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TI UT WOS:000282192900061 ER PT J AU Su, YN van Ballegooijen, A Golub, L AF Su, Yingna van Ballegooijen, Adriaan Golub, Leon TI STRUCTURE AND DYNAMICS OF QUIESCENT FILAMENT CHANNELS OBSERVED BY HINODE/XRT AND STEREO/EUVI SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: corona; Sun: filaments, prominences; Sun: magnetic topology; Sun: UV radiation; Sun: X-rays, gamma rays ID GLOBAL SOLAR CORONA; ACTIVE-REGION 10953; RAY TELESCOPE XRT; MAGNETIC-FIELDS; H-ALPHA; FLUX ROPE; PROMINENCES; EVOLUTION; SUN; SIMULATIONS AB We present a study of the structure and dynamics of quiescent filament channels observed by Hinode/XRT and STEREO/EUVI at the solar minimum 23/24 from 2006 November to 2008 December. For 12 channels identified on the solar disk (Group I channels), we find that the morphology of the structure on the two sides of the channel is asymmetric in bothX-rays and EUV: the eastern side has curved features while the western side has straight features. We interpret the results in terms of a magnetic flux rope model. The asymmetry in the morphology is due to the variation in axial flux of the flux rope along the channel, which causes the field lines from one polarity to turn into the flux rope (curved feature), while the field lines from the other polarity are connected to very distant sources (straight). For most of the 68 channels identified by cavities at the east and west limbs (Group II channels), the asymmetry cannot be clearly identified, which is likely due to the fact that the axial flux may be relatively constant along such channels. Corresponding cavities are identified only for 5 of the 12 Group I channels, while Group II channels are identified for all of the 68 cavity pairs. The studied filament channels are often observed as dark channels in X-rays and EUV. Sheared loops within Group I channels are often seen in X-rays, but are rarely seen in Group II channels as shown in the X-ray Telescope daily synoptic observations. A survey of the dynamics of studied filament channels shows that filament eruptions occur at an average rate of 1.4 filament eruptions per channel per solar rotation. C1 [Su, Yingna; van Ballegooijen, Adriaan; Golub, Leon] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Su, YN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ynsu@head.cfa.harvard.edu RI Su, Yingna/J-1674-2012; OI van Ballegooijen, Adriaan/0000-0002-5622-3540; Golub, Leon/0000-0001-9638-3082 FU NASA [NNM07AB07C]; International Space Science Institute (Bern) FX We thank the referee for helpful comments to improve this paper. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and the NSC (Norway). The authors thank the teams of Hinode/XRT, STEREO/SECCHI, Yohkoh/SXT, TRACE, SOLIS, SOHO/LASCO, KSO, MLSO, BBSO for providing the valuable data. US members of the XRT team are supported by NASA contract NNM07AB07C to Smithsonian Astrophysical Observatory (SAO). Y.S. acknowledges Dr. Kathy Reeves and Dr. David McKenzie for providing observational information on cavities and filament channels by Hinode/XRT and Yohkoh/SXT. The authors acknowledge the International Space Science Institute (Bern) for supporting the international team on Prominence Cavities. They also thank the team members for lively discussions. NR 53 TC 9 Z9 9 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2010 VL 721 IS 1 BP 901 EP 910 DI 10.1088/0004-637X/721/1/901 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654TI UT WOS:000282192900069 ER PT J AU Kewley, LJ Rupke, D Zahid, HJ Geller, MJ Barton, EJ AF Kewley, Lisa J. Rupke, David Zahid, H. Jabran Geller, Margaret J. Barton, Elizabeth J. TI METALLICITY GRADIENTS AND GAS FLOWS IN GALAXY PAIRS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: abundances; galaxies: fundamental parameters; galaxies: interactions; galaxies: starburst ID TRIGGERED STAR-FORMATION; ULTRALUMINOUS INFRARED GALAXIES; GEMINI SPECTROSCOPIC SURVEY; EXTRAGALACTIC HII-REGIONS; CLOSE PAIRS; ABUNDANCE GRADIENT; STARBURST GALAXIES; MOLECULAR GAS; H-II; CLUSTERS AB We present the first systematic investigation into the metallicity gradients in galaxy close pairs. We determine the metallicity gradients for eight galaxies in close pairs using H II region metallicities obtained with high signal-to-noise multi-slit observations with the Keck LRIS Spectrograph. We show that the metallicity gradients in close pairs are significantly shallower than gradients in isolated spiral galaxies such as the Milky Way, M83, and M101. These observations provide the first solid evidence that metallicity gradients in interacting galaxies are systematically different from metallicity gradients in isolated spiral galaxies. Our results suggest that there is a strong relationship between metallicity gradients and the gas dynamics in galaxy interactions and mergers. C1 [Kewley, Lisa J.; Rupke, David; Zahid, H. Jabran] Univ Hawaii, Inst Astron, Hilo, HI 96822 USA. [Geller, Margaret J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Barton, Elizabeth J.] Univ Calif Irvine, Irvine, CA 92697 USA. RP Kewley, LJ (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Hilo, HI 96822 USA. EM kewley@ifa.hawaii.edu NR 50 TC 87 Z9 87 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 20 PY 2010 VL 721 IS 1 BP L48 EP L52 DI 10.1088/2041-8205/721/1/L48 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647HY UT WOS:000281610300011 ER PT J AU Horton, BM Yoon, J Ghalambor, CK Moore, IT Sillett, TS AF Horton, Brent M. Yoon, Jongmin Ghalambor, Cameron K. Moore, Ignacio T. Sillett, T. Scott TI Seasonal and population variation in male testosterone levels in breeding orange-crowned warblers (Vermivora celata) SO GENERAL AND COMPARATIVE ENDOCRINOLOGY LA English DT Article DE Breeding density; Life history; Mating effort; Parental investment; Testosterone Trade-offs ID DARK-EYED JUNCOS; EXPERIMENTALLY ELEVATED TESTOSTERONE; IMMUNOCOMPETENCE HANDICAP HYPOTHESIS; AVIAN LIFE HISTORIES; BASAL METABOLIC-RATE; MALE HOUSE SPARROWS; MALE GREAT TITS; TRADE-OFFS; BEHAVIORAL INSENSITIVITY; TERRITORIAL BEHAVIOR AB Comparative hormone studies can reveal how physiology underlies life history variation. Here, we examined seasonal variation in plasma testosterone concentration between populations of male orangecrowned warblers (Vermivora celata) breeding in Fairbanks, Alaska (V. c. celata) and on Santa Catalina Island, California (V. c. sordida). These populations face different ecological constraints and exhibit different life histories. Alaska birds have a short breeding season, low annual adult survival, and high reproductive rates. In contrast, Catalina Island birds exhibit high adult survival and low reproductive rates despite having a long breeding season. We examined seasonal variation in male testosterone concentrations as a potential mechanism underlying differences in male reproductive strategies between populations. From 2006 to 2008, we sampled males during the pre-incubation, incubation, and nestling stages. Alaska males exhibited a seasonal testosterone pattern typical of northern passerines: testosterone levels were high during pre-incubation and declined during incubation to low levels during nestling provisioning. Testosterone concentrations in Catalina Island males, however, did not vary consistently with breeding stage, remained elevated throughout the breeding season, and were higher than in Alaska males during the nestling stage. We hypothesize that in Alaska, where short seasons and high adult mortality limit breeding opportunities, the seasonal testosterone pattern facilitates high mating effort prior to incubation, but high parental investment during the nestling stage. On Catalina Island, elevated testosterone levels may reflect the extended mating opportunities and high population density facing males in this population. Our results suggest that population variation in seasonal testosterone patterns in orange-crowned warblers may be a function of differences in life history strategy and the social environment. Published by Elsevier Inc. C1 [Horton, Brent M.; Sillett, T. Scott] Smithsonian Migratory Bird Ctr, Washington, DC 20013 USA. [Yoon, Jongmin; Ghalambor, Cameron K.] Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. [Moore, Ignacio T.] Virginia Tech, Dept Biol Sci, Blacksburg, VA 24061 USA. RP Horton, BM (reprint author), Smithsonian Migratory Bird Ctr, Natl Zool Pk,POB 37012 MRC 5503, Washington, DC 20013 USA. EM hortonb@si.edu OI Moore, Ignacio/0000-0001-8875-8913 NR 74 TC 15 Z9 15 U1 0 U2 18 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0016-6480 J9 GEN COMP ENDOCR JI Gen. Comp. Endocrinol. PD SEP 15 PY 2010 VL 168 IS 3 BP 333 EP 339 DI 10.1016/j.ygcen.2010.04.019 PG 7 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 641LF UT WOS:000281126700005 PM 20420840 ER PT J AU Aplin, KP Helgen, KM Lunde, DP AF Aplin, Kenneth P. Helgen, Kristofer M. Lunde, Darrin P. TI A Review of Peroryctes broadbenti, the Giant Bandicoot of Papua New Guinea SO AMERICAN MUSEUM NOVITATES LA English DT Review ID SEXUAL-DIMORPHISM; CANINE SIZE; MARSUPIALIA; MAMMALS; PERAMELEMORPHIA; THYLACOMYIDAE; POPULATIONS; SELECTION; BEHAVIOR; MURIDAE AB The giant bandicoot, Peroryctes broadbenti (Ramsay, 1879), is represented in museum collections by 23 specimens collected at 12 localities in the lowlands of the southeastern peninsula (the "Papuan Peninsula") of Papua New Guinea. Available data on P broadbenti are reviewed, including its comparative anatomy and morphological variability, taxonomic relationships, geographic and elevational distribution, dietary and reproductive traits, and conservation status. Despite previous confusion between this species and P. raffrayana (Milne-Edwards, 1878), the two species are readily distinguished by a suite of external, cranial, and dental characters. Diagnostic characters are enumerated and illustrated, and comparisons drawn with other New Guinean bandicoots. Generic distinction of Peroryctes Thomas, 1906, in cranial morphology from other New Guinean bandicoots is also reviewed. A striking degree of sexual dimorphism is documented in both body size and dentition for P broadbenti; these comparisons are set in context by a review of sexual dimorphism among bandicoots in general. C1 [Aplin, Kenneth P.] CSIRO, Div Sustainable Ecosyst, Canberra, ACT 2601, Australia. [Aplin, Kenneth P.; Helgen, Kristofer M.; Lunde, Darrin P.] Amer Museum Nat Hist, Div Vertebrate Zool Mammal, New York, NY 10024 USA. [Helgen, Kristofer M.] Smithsonian Inst, Div Mammals, Natl Museum Nat Hist, MRC 108, Washington, DC 20013 USA. RP Aplin, KP (reprint author), CSIRO, Div Sustainable Ecosyst, Canberra, ACT 2601, Australia. EM ken.aplin@csiro.au; helgenk@si.edu; lunde@amnh.org FU Smithsonian Institution; National Science Foundation; Bernice P. Bishop Museum; American Society of Mammalogists FX The second author's studies of New Guinean mammals were supported by grants from the Smithsonian Institution, National Science Foundation, the Bernice P. Bishop Museum, and the American Society of Mammalogists. NR 86 TC 16 Z9 16 U1 0 U2 5 PU AMER MUSEUM NATURAL HISTORY PI NEW YORK PA ATTN: LIBRARY-SCIENTIFIC PUBLICATIONS DISTRIBUTION, CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024-5192 USA SN 0003-0082 EI 1937-352X J9 AM MUS NOVIT JI Am. Mus. Novit. PD SEP 14 PY 2010 IS 3696 BP 1 EP 41 PG 41 WC Biodiversity Conservation; Zoology SC Biodiversity & Conservation; Zoology GA 650QU UT WOS:000281866700001 ER PT J AU Garcia-Robledo, C Horvitz, CC Staines, CL AF Garcia-Robledo, Carlos Horvitz, Carol C. Staines, Charles L. TI Larval morphology, development, and notes on the natural history of Cephaloleia "rolled-leaf" beetles (Coleoptera: Chrysomelidae: Cassidinae) SO ZOOTAXA LA English DT Article DE Cannaceae; Cephaloleia; Costaceae; Heliconiaceae; Larval development; life cycle; Marantaceae; sexual dimorphism; Zingiberaceae; Zingiberales ID HELICONIA INSECT COMMUNITIES; HISPINE BEETLES; HERBIVORES; EVOLUTION; GINGERS; FOREST; ZINGIBERALES; IMBRICATA; CHEMISTRY AB The Neotropical genus Cephaloleia Chevrolat, 1837 is comprised of 209 described species. Adults usually feed and mate within the scrolls formed by the young rolled leaves of plants of Neotropical Zingiberales. This paper reports for populations of Cephaloleia belti Baly, C. dilaticollis Baly, C. dorsalis Baly and C. placida Baly at La Selva Biological Station (Costa Rica, Central America) detailed descriptions of: 1. larval and adult diets and diet breadth; 2. egg, larval and pupal morphology; 3. larval development times; 4. dimorphic sexual characteristics; 5. adult longevity; and 6. differences in lifespan between genders. Cephaloleia belti displays the broader diet breadth, feeding on 14 species of three families of Zingiberales. Cephaloleia dilaticollis feeds on nine species of three families of Zingiberales. Cephaloleia dorsalis and C. placida feed on four species of Costaceae and two species of Zingiberaceae, respectively. Time to pupation ranges among species from 32.8 to 59.1 days. In the four Cephaloleia species, adult females are larger than males. Genders display marked sexual dimorphism in the shape of their last abdominal sternite and the pygidium. Longevity of adults ranged from ca. 300 to 390 days. Life expectancy estimates for adult beetles reared in the laboratory ranged from 111.5 to 187.2 days. Male and female adults of C. belti and C. dilaticollis have equivalent life expectancies. However, life expectancy is longer for male C. dorsalis and C. placida. C1 [Garcia-Robledo, Carlos; Horvitz, Carol C.] Univ Miami, Dept Biol, Coral Gables, FL 33124 USA. [Staines, Charles L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Garcia-Robledo, C (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, POB 37012, Washington, DC 20013 USA. EM garciac@si.edu FU University of Miami; OTS (Organization for Tropical Studies); College of Arts and Sciences, University of Miami FX The authors thank the staff of La Selva Biological Station - Organization for Tropical Studies. We want to thank G. Frias, J.G. Huertas, G. Huertas and R. Sanchez, for assistance in the field and laboratory. SEM images were provided by P. Blackwelder, H. Al Sayegh, and X. Vial - University of Miami Center for Advanced Microscopy (UMCAM). The illustrations included in this paper were made by E. K. Kuprewicz. This research was funded by the J. McLamore Fellowship - University of Miami and the OTS (Organization for Tropical Studies) - Donald and Beverly Stone Fellowship and the OTS-Christiane and Christopher Tyson Fellowship to C. Garcia-Robledo and the Cooper Fellowship, College of Arts and Sciences, University of Miami to C. C. Horvitz. Comments by M. L. Chamorro-Lacayo, T. H. Fleming, D. J. Futuyma, J. Gomez-Zurita, E. K. Kuprewicz, K. D. Waddington, B. A. Whitlock and two anonymous reviewers improved this manuscript substantially. This is contribution No. 663 of the Program in Tropical Biology, Evolution and Behavior, Department of Biology, University of Miami. NR 53 TC 14 Z9 14 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD SEP 13 PY 2010 IS 2610 BP 50 EP 68 PG 19 WC Zoology SC Zoology GA 648TZ UT WOS:000281718500003 ER PT J AU Younger, JD Fazio, GG Ashby, MLN Civano, F Gurwell, MA Huang, JS Iono, D Peck, AB Petitpas, GR Scott, KS Wilner, DJ Wilson, GW Yun, MS AF Younger, Joshua D. Fazio, Giovanni G. Ashby, Matthew L. N. Civano, Francesca Gurwell, Mark A. Huang, Jia-Sheng Iono, Daisuke Peck, Alison B. Petitpas, Glen R. Scott, Kimberly S. Wilner, David J. Wilson, Grant W. Yun, Min S. TI The physical scale of the far-infrared emission in the most luminous submillimetre galaxies - II. Evidence for merger-driven star formation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE instrumentation: interferometers; galaxies: high-redshift; galaxies: interactions; galaxies: starburst; infrared: galaxies; submillimetre: general ID SUPERMASSIVE BLACK-HOLES; ACTIVE GALACTIC NUCLEI; HIGH-REDSHIFT GALAXIES; INITIAL MASS FUNCTION; PHASE CALIBRATION SOURCES; EVOLUTION SURVEY COSMOS; LAMBDA-CDM UNIVERSE; MU-M OBSERVATIONS; FORMING GALAXIES; RADIO CORRELATION AB We present high-resolution 345-GHz interferometric observations of two extremely luminous (L(ir) greater than or similar to 1013 L(circle dot)), submillimetre-selected galaxies (SMGs) in the Cosmic Evolution Survey (COSMOS) field with the Submillimeter Array (SMA). Both targets were previously detected as unresolved point sources by the SMA in its compact configuration, also at 345 GHz. These new data, which provide a factor of greater than or similar to 3 improvement in resolution, allow us to measure the physical scale of the far-infrared in the submillimetre directly. The visibility functions of both targets show significant evidence for structure on similar to 0.5-1-arcsec scales, which at z greater than or similar to 1.5 translates into a physical scale of similar to 5-8 kpc. Our results are consistent with the angular and physical scales of two comparably luminous objects with high-resolution SMA follow-up, as well as radio continuum and CO sizes of other SMGs. These relatively compact sizes (less than or similar to 5-10 kpc) argue strongly for merger-driven starbursts, rather than extended gas-rich discs, as the preferred channel for forming SMGs. C1 [Younger, Joshua D.] Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA. [Fazio, Giovanni G.; Ashby, Matthew L. N.; Civano, Francesca; Gurwell, Mark A.; Huang, Jia-Sheng; Petitpas, Glen R.; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Iono, Daisuke] Nobeyama Radio Observ, Minamisa Ku, Nagano 3841805, Japan. [Peck, Alison B.] Joint ALMA Off, Santiago 7550108, Chile. [Scott, Kimberly S.; Wilson, Grant W.; Yun, Min S.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Scott, Kimberly S.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. RP Younger, JD (reprint author), Inst Adv Study, Sch Nat Sci, Einstein Dr, Princeton, NJ 08540 USA. EM jyounger@ias.edu FU Smithsonian Institution; Academia Sinica; NASA [HF-51266.01, NAS 5-26555, HST-GO-09822]; NSF [AST 0828222, AST 0907952] FX We are thankful to the referee for his helpful comments. The Sub-millimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. This research has made use of data obtained from the Chandra Data Archive and software provided by the Chandra X-ray Center (CXC) in the application packages CIAO and SHERPA. This research was based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan, as well as observations obtained with WIRCam, a joint project of Canada-France-Hawaii Telescope (CFHT), Taiwan, Korea, Canada, France and the CFHT which is operated by the National Research Council (NRC) of Canada, the Institute National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France and the University of Hawaii. We furthermore utilize observations made with the NASA/ESA HST. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc., and the James Clerk Maxwell Telescope is operated by The Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the Netherlands Organisation for Scientific Research and the National Research Council of Canada. JDY acknowledges support from NASA through Hubble Fellowship grant HF-51266.01 awarded by the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. STScI is operated by the association of Universities for Research in Astronomy, Inc., under the NASA contract NAS 5-26555. The HST COSMOS Treasury programme was supported through NASA grant HST-GO-09822. Work with the AzTEC data is supported, in part, by NSF grants AST 0828222 and AST 0907952. NR 156 TC 25 Z9 25 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 11 PY 2010 VL 407 IS 2 BP 1268 EP 1276 DI 10.1111/j.1365-2966.2010.16984.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 646OG UT WOS:000281551300045 ER PT J AU Sato, M Reid, MJ Brunthaler, A Menten, KM AF Sato, M. Reid, M. J. Brunthaler, A. Menten, K. M. TI TRIGONOMETRIC PARALLAX OF W51 MAIN/SOUTH SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; Galaxy: fundamental parameters; Galaxy: kinematics and dynamics; Galaxy: structure; ISM: individual objects (W51); masers ID H2O MASER SOURCES; STAR-FORMING REGION; CELESTIAL REFERENCE FRAME; GHZ METHANOL MASERS; PROPER MOTIONS; MASSIVE CORES; ORION-KL; DYNAMICAL COLLAPSE; STELLAR ORBITS; SPIRAL ARM AB We report measurement of the trigonometric parallax of W51 Main/South using the Very Long Baseline Array. We measure a value of 0.185 +/- 0.010 mas corresponding to a distance of 5.41(-0.28)(+0.31) kpc. W51 Main/South is a well-known massive star-forming region near the tangent point of the Sagittarius spiral arm of the Milky Way. Our distance to W51 yields an estimate of the distance to the Galactic center of R(0) = 8.3 +/- 0.46 (statistical) +/-1.0 (systematic) kpc by simple geometry. Combining the parallax and proper motion measurements for W51, we obtained the full-space motion of thismassive star-forming region. We find W51 is in a nearly circular orbit about the Galactic center. The H(2)O masers used for our parallax measurements trace four powerful bipolar outflows within a 0.4 pc size region, some of which are associated with dusty molecular hot cores and/or hyper- or ultra-compact HII regions. C1 [Sato, M.] Univ Tokyo, Grad Sch Sci, Dept Astron, Tokyo 1130033, Japan. [Sato, M.; Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sato, M.] Natl Inst Nat Sci, Natl Astron Observ Japan, VERA Project, Mitaka, Tokyo 1818588, Japan. [Brunthaler, A.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Sato, M (reprint author), Univ Tokyo, Grad Sch Sci, Dept Astron, Tokyo 1130033, Japan. FU JSPS FX The authors thank an anonymous referee for many valuable comments. M. S. acknowledges financial support from the JSPS Research Fellowships for Young Scientists. This work was supported by a Grant-in-Aid for JSPS Fellows and conducted as part of her visiting research at Harvard-Smithsonian Center for Astrophysics through Smithsonian Astrophysical Observatory Predoctoral Program and the JSPS Excellent Young Researchers Overseas Visit Program. NR 60 TC 85 Z9 85 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2010 VL 720 IS 2 BP 1055 EP 1065 DI 10.1088/0004-637X/720/2/1055 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647ND UT WOS:000281624300009 ER PT J AU Cavagnolo, KW McNamara, BR Nulsen, PEJ Carilli, CL Jones, C Birzan, L AF Cavagnolo, K. W. McNamara, B. R. Nulsen, P. E. J. Carilli, C. L. Jones, C. Birzan, L. TI A RELATIONSHIP BETWEEN AGN JET POWER AND RADIO POWER SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: clusters: general; radio continuum: galaxies; X-rays: galaxies ID ACTIVE GALACTIC NUCLEUS; EARLY-TYPE GALAXIES; HOT INTERSTELLAR-MEDIUM; X-RAY BINARIES; CHANDRA OBSERVATIONS; BLACK-HOLES; SKY-SURVEY; ELLIPTIC GALAXIES; SCALING RELATION; BUOYANT BUBBLES AB Using Chandra X-ray and Very Large Array radio data, we investigate the scaling relationship between jet power, P(jet), and synchrotron luminosity, P(radio). We expand the sample presented in Birzan et al. to lower radio power by incorporating measurements for 21 giant elliptical galaxies (gEs) to determine if the Birzan et al. P(jet)-P(radio) scaling relations are continuous in form and scatter from gEs up to brightest cluster galaxies. We find a mean scaling relation of P(jet) approximate to 5.8 x 10(43) (P(radio)/10(40))(0.70) erg s(-1) which is continuous over similar to 6-8 decades in P(jet) and P(radio) with a scatter of approximate to 0.7 dex. Our mean scaling relationship is consistent with the model presented in Willott et al. if the typical fraction of lobe energy in non-radiating particles to that in relativistic electrons is greater than or similar to 100. We identify several gEs whose radio luminosities are unusually large for their jet powers and have radio sources which extend well beyond the densest parts of their X-ray halos. We suggest that these radio sources are unusually luminous because they were unable to entrain appreciable amounts of gas. C1 [Cavagnolo, K. W.; McNamara, B. R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [McNamara, B. R.; Nulsen, P. E. J.; Jones, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Carilli, C. L.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Birzan, L.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Cavagnolo, KW (reprint author), Univ Waterloo, Dept Phys & Astron, 200 Univ Ave W, Waterloo, ON N2L 3G1, Canada. EM kcavagno@uwaterloo.ca OI Nulsen, Paul/0000-0003-0297-4493 FU CXO; CXO Center; NASA [NAS8-03060] FX K. W. C. and B. R. M. acknowledge generous support from the Natural Sciences and Engineering Research Council of Canada and grants from the CXO. C.J. thanks the Smithsonian Institution for generous support. P.N. thanks the CXO Center for supporting this work. K. W. C. thanks Judith Croston, David Rafferty, Lorant Sjouwerman, and Chris Willott for helpful discussions. We also thank the anonymous referee for a prompt and helpful review. The CXO Center is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 71 TC 137 Z9 137 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2010 VL 720 IS 2 BP 1066 EP 1072 DI 10.1088/0004-637X/720/2/1066 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647ND UT WOS:000281624300010 ER PT J AU Buchhave, LA Bakos, GA Hartman, JD Torres, G Kovacs, G Latham, DW Noyes, RW Esquerdo, GA Everett, M Howard, AW Marcy, GW Fischer, DA Johnson, JA Andersen, J Furesz, G Perumpilly, G Sasselov, DD Stefanik, RP Beky, B Lazar, J Papp, I Sari, P AF Buchhave, L. A. Bakos, G. A. Hartman, J. D. Torres, G. Kovacs, G. Latham, D. W. Noyes, R. W. Esquerdo, G. A. Everett, M. Howard, A. W. Marcy, G. W. Fischer, D. A. Johnson, J. A. Andersen, J. Furesz, G. Perumpilly, G. Sasselov, D. D. Stefanik, R. P. Beky, B. Lazar, J. Papp, I. Sari, P. TI HAT-P-16b: A 4 M-J PLANET TRANSITING A BRIGHT STAR ON AN ECCENTRIC ORBIT SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HAT-P-16, GSC 2792-01700); techniques: photometric; techniques: spectroscopic ID COROT SPACE MISSION; EXTRASOLAR PLANETS; TIDAL EVOLUTION; PERIOD PLANETS; K STAR; STELLAR; ALGORITHM; FIELD; SPECTROSCOPY; EXOPLANETS AB We report the discovery of HAT-P-16b, a transiting extrasolar planet orbiting the V = 10.8mag F8 dwarf GSC 279201700, with a period P = 2.775960 +/- 0.000003 days, transit epoch T-c = 2455027.59293 +/- 0.00031 (BJD10), and transit duration 0.1276 +/- 0.0013 days. The host star has a mass of 1.22 +/- 0.04 (M)circle dot, radius of 1.24 +/- 0.05 R-circle dot, effective temperature 6158 +/- 80 K, and metallicity [Fe/H] = + 0.17 +/- 0.08. The planetary companion has a mass of 4.193 +/- 0.094 M-J and radius of 1.289 +/- 0.066 R-J, yielding a mean density of 2.42 +/- 0.35 g cm(-3). Comparing these observed characteristics with recent theoretical models, we find that HAT-P-16b is consistent with a 1 Gyr H/He-dominated gas giant planet. HAT-P-16b resides in a sparsely populated region of the mass-radius diagram and has a non-zero eccentricity of e = 0.036 with a significance of 10s. C1 [Buchhave, L. A.; Bakos, G. A.; Hartman, J. D.; Torres, G.; Latham, D. W.; Noyes, R. W.; Esquerdo, G. A.; Everett, M.; Furesz, G.; Perumpilly, G.; Sasselov, D. D.; Stefanik, R. P.; Beky, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buchhave, L. A.; Andersen, J.] Univ Copenhagen, Niels Bohr Inst, DK-1168 Copenhagen, Denmark. [Kovacs, G.] Konkoly Observ Budapest, Budapest, Hungary. [Howard, A. W.; Marcy, G. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Fischer, D. A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Johnson, J. A.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Andersen, J.] Nord Opt Telescope Sci Assoc, La Palma, Canary Islands, Spain. [Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary. RP Buchhave, LA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Buchhave, Lars A./0000-0003-1605-5666; Hartman, Joel/0000-0001-8732-6166; Fischer, Debra/0000-0003-2221-0861 FU NASA [NNG04GN74G, NNX08AF23G, NNX09AF59G, NCC2-1390, N018Hr]; SAO IRD; NSF [AST-0702843, AST-0702821]; Hungarian Scientific Research Foundation (OTKA) [K-81373] FX HATNet operations have been funded by NASA grants NNG04GN74G, NNX08AF23G, and SAO IR&D grants. The work of G.A.B. and J.A.J. were supported by the Postdoctoral Fellowship of the NSF Astronomy and Astrophysics Program (AST-0702843 and AST-0702821, respectively). G. T. acknowledges partial support from NASA grant NNX09AF59G. We acknowledge partial support also from the Kepler Mission under NASA Cooperative Agreement NCC2-1390 ( D. W. L., PI). G. K. thanks the Hungarian Scientific Research Foundation (OTKA) for support through grant K-81373. Based in part on observations made with the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This research has made use of Keck telescope time granted through NASA (N018Hr). NR 48 TC 101 Z9 101 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2010 VL 720 IS 2 BP 1118 EP 1125 DI 10.1088/0004-637X/720/2/1118 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647ND UT WOS:000281624300015 ER PT J AU Acciari, VA Arlen, T Aune, T Beilicke, M Benbow, W Boltuch, D Bradbury, SM Buckley, JH Bugaev, V Byrum, K Cannon, A Cesarini, A Christiansen, JL Ciupik, L Cui, W Dickherber, R Duke, C Finley, JP Finnegan, G Furniss, A Galante, N Godambe, S Grube, J Guenette, R Gyuk, G Hanna, D Holder, J Hui, CM Humensky, TB Imran, A Kaaret, P Karlsson, N Kertzman, M Kieda, D Konopelko, A Krawczynski, H Krennrich, F Maier, G McArthur, S McCann, A McCutcheon, M Moriarty, P Ong, RA Otte, AN Pandel, D Perkins, JS Pohl, M Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Rose, HJ Schroedter, M Sembroski, GH Senturk, GD Smith, AW Steele, D Swordy, SP Tesic, G Theiling, M Thibadeau, S Varlotta, A Vassiliev, VV Vincent, S Wagner, RG Wakely, SP Ward, JE Weekes, TC Weinstein, A Weisgarber, T Williams, DA Wissel, S Zitzer, B AF Acciari, V. A. Arlen, T. Aune, T. Beilicke, M. Benbow, W. Boltuch, D. Bradbury, S. M. Buckley, J. H. Bugaev, V. Byrum, K. Cannon, A. Cesarini, A. Christiansen, J. L. Ciupik, L. Cui, W. Dickherber, R. Duke, C. Finley, J. P. Finnegan, G. Furniss, A. Galante, N. Godambe, S. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Holder, J. Hui, C. M. Humensky, T. B. Imran, A. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Konopelko, A. Krawczynski, H. Krennrich, F. Maier, G. McArthur, S. McCann, A. McCutcheon, M. Moriarty, P. Ong, R. A. Otte, A. N. Pandel, D. Perkins, J. S. Pohl, M. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Rose, H. J. Schroedter, M. Sembroski, G. H. Senturk, G. Demet Smith, A. W. Steele, D. Swordy, S. P. Tesic, G. Theiling, M. Thibadeau, S. Varlotta, A. Vassiliev, V. V. Vincent, S. Wagner, R. G. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Weisgarber, T. Williams, D. A. Wissel, S. Zitzer, B. TI VERITAS SEARCH FOR VHE GAMMA-RAY EMISSION FROM DWARF SPHEROIDAL GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies: dwarf; gamma rays: galaxies ID EXPLORING HALO SUBSTRUCTURE; DARK-MATTER SUBSTRUCTURE; VELOCITY DISPERSION PROFILES; MILKY-WAY HALO; URSA-MINOR; GIANT STARS; DENSITY PROFILES; GALACTIC-CENTER; DRACO; TELESCOPE AB Indirect dark matter searches with ground-based gamma-ray observatories provide an alternative for identifying the particle nature of dark matter that is complementary to that of direct search or accelerator production experiments. We present the results of observations of the dwarf spheroidal galaxies Draco, Ursa Minor, Bootes 1, and Willman 1 conducted by the Very Energetic Radiation Imaging Telescope Array System (VERITAS). These galaxies are nearby dark matter dominated objects located at a typical distance of several tens of kiloparsecs for which there are good measurements of the dark matter density profile from stellar velocity measurements. Since the conventional astrophysical background of very high energy gamma rays from these objects appears to be negligible, they are good targets to search for the secondary gamma-ray photons produced by interacting or decaying dark matter particles. No significant gamma-ray flux above 200 GeV was detected from these four dwarf galaxies for a typical exposure of similar to 20 hr. The 95% confidence upper limits on the integral gamma-ray flux are in the range (0.4-2.2) x 10(-12) photons cm(-2) s(-1). We interpret this limiting flux in the context of pair annihilation of weakly interacting massive particles (WIMPs) and derive constraints on the thermally averaged product of the total self-annihilation cross section and the relative velocity of the WIMPs ( less than or similar to 10(-23) cm(3) s(-1) for m(chi) greater than or similar to 300 GeV c(-2)). This limit is obtained under conservative assumptions regarding the dark matter distribution in dwarf galaxies and is approximately 3 orders of magnitude above the generic theoretical prediction for WIMPs in the minimal supersymmetric standard model framework. However, significant uncertainty exists in the dark matter distribution as well as the neutralino cross sections which under favorable assumptions could further lower this limit. C1 [Acciari, V. A.; Benbow, W.; Galante, N.; Perkins, J. S.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Arlen, T.; Ong, R. A.; Vassiliev, V. V.; Weinstein, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Boltuch, D.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Boltuch, D.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Byrum, K.; Smith, A. W.; Wagner, R. G.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cannon, A.; Quinn, J.; Ward, J. E.] Natl Univ Ireland Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cesarini, A.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Christiansen, J. L.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Ciupik, L.; Grube, J.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cui, W.; Finley, J. P.; Sembroski, G. H.; Varlotta, A.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Finnegan, G.; Godambe, S.; Hui, C. M.; Kieda, D.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; McCutcheon, M.; Ragan, K.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Humensky, T. B.; Swordy, S. P.; Wakely, S. P.; Weisgarber, T.; Wissel, S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Imran, A.; Krennrich, F.; Pohl, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kaaret, P.; Pandel, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Senturk, G. Demet] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. RP Acciari, VA (reprint author), Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. EM rgwcdf@hep.anl.gov OI Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610; Ward, John E/0000-0003-1973-0794; Pandel, Dirk/0000-0003-2085-5586 FU US National Science Foundation; US Department of Energy; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland; STFC in the UK; U.S. National Science Foundation [0422093] FX This research is supported by grants from the US National Science Foundation, the US Department of Energy, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland, and by STFC in the UK. We acknowledge the excellent work of the technical support staff at the FLWO and the collaborating institutions in the construction and operation of the instrument. V. V. V. acknowledges the support of the U.S. National Science Foundation under CAREER program (Grant No. 0422093). NR 71 TC 59 Z9 59 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2010 VL 720 IS 2 BP 1174 EP 1180 DI 10.1088/0004-637X/720/2/1174 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647ND UT WOS:000281624300021 ER PT J AU Hung, LW Hickox, RC Boroson, BS Vrtilek, SD AF Hung, Li-Wei Hickox, Ryan C. Boroson, Bram S. Vrtilek, Saeqa D. TI SUZAKU X-RAY SPECTRA AND PULSE PROFILE VARIATIONS DURING THE SUPERORBITAL CYCLE OF LMC X-4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; pulsars: individual (LMC X-4); stars: neutron; X-rays: binaries ID PHASE RESOLVED-SPECTROSCOPY; NEUTRON-STAR; XMM-NEWTON; TIMING-EXPLORER; ORBITAL DECAY; SMC X-1; PERIOD; ACCRETION; DISCOVERY; HERCULES-X-1 AB We present results from spectral and temporal analyses of Suzaku and RXTE observations of the high-mass X-ray binary LMC X-4. Using the full 13 years of available RXTE/all-sky monitor data, we apply the ANOVA and Lomb Normalized Periodogram methods to obtain an improved superorbital period measurement of 30.32 +/- 0.04 days. The phase-averaged X-ray spectra from Suzaku observations during the high state of the superorbital period can be modeled in the 0.6-50 keV band as the combination of a power law with Gamma similar to 0.6 and a highenergy cutoff at similar to 25 keV, a blackbody with kT(BB) similar to 0.18 keV, and emission lines from Fe K-alpha, OVIII, and NeIX (x Ly alpha). Assuming a distance of 50 kpc, the source has luminosity L-X similar to 3 x 10(38) erg s(-1) in the 2-50 keV band, and the luminosity of the soft (blackbody) component is L-BB similar to 1.5 x 10(37) erg s-1. The energy-resolved pulse profiles show single-peaked soft (0.5-1 keV) and hard (6-10 keV) pulses but a more complex pattern of medium (2-10 keV) pulses; cross-correlation of the hard with the soft pulses shows a phase shift that varies between observations. We interpret these results in terms of a picture in which a precessing disk reprocesses the hard X-rays and produces the observed soft spectral component, as has been suggested for the similar sources Her X-1 and SMC X-1. C1 [Hung, Li-Wei] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Hung, Li-Wei; Hickox, Ryan C.; Boroson, Bram S.; Vrtilek, Saeqa D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hickox, Ryan C.] Univ Durham, Dept Phys, Durham DH1 3LE, England. RP Hung, LW (reprint author), Ohio State Univ, Dept Astron, McPherson Lab 140 W 18th Ave, Columbus, OH 43210 USA. EM hung.88@buckeyemail.osu.edu; rhickox@cfa.harvard.edu; bboroson@cfa.harvard.edu; svrtilek@cfa.harvard.edu RI XRAY, SUZAKU/A-1808-2009 FU National Science Foundation; Department of Defense [0754568]; Suzaku [NNX08AI17G]; ADP [NNX08AJ61G]; Smithsonian Institution FX We are grateful to Joseph Neilsen for his contribution to the data analysis, and to Chris Done, Christine Jones, Jonathan McDowell, and Marie Machacek for helpful discussions. We also thank the Suzaku Helpdesk for their valuable advice on the data analysis. The work was supported in part by the National Science Foundation Research Experiences for Undergraduates (REU) and Department of Defense Awards to Stimulate and Support Undergraduate Research Experiences (ASSURE) programs under grant 0754568, Suzaku grant NNX08AI17G, ADP grant NNX08AJ61G, and by the Smithsonian Institution. R. C. H. was supported by an SAO Postdoctoral Fellowship and an STFC Postdoctoral Fellowship. NR 48 TC 8 Z9 8 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2010 VL 720 IS 2 BP 1202 EP 1214 DI 10.1088/0004-637X/720/2/1202 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647ND UT WOS:000281624300023 ER PT J AU Rodriguez, DR Kastner, JH Wilner, D Qi, CH AF Rodriguez, David R. Kastner, Joel H. Wilner, David Qi, Chunhua TI IMAGING THE MOLECULAR DISK ORBITING THE TWIN YOUNG SUNS OF V4046 Sgr SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: spectroscopic; circumstellar matter; planetary systems; radio lines: stars; stars: individual (V4046 Sgr); stars: pre-main sequence ID PROTOPLANETARY DISKS; CIRCUMSTELLAR DISKS; H-2 EMISSION; SUBMILLIMETER ARRAY; STELLAR COMPANIONS; ORGANIC-MOLECULES; PLANET FORMATION; KEPLERIAN DISK; BINARY-SYSTEMS; STAR-FORMATION AB We have imaged the disk surrounding the nearby (D similar to 73 pc), similar to 12 Myr, classical T Tauri binary system V4046 Sgr with the Submillimeter Array (SMA) at an angular resolution of similar to 2 ''. We detect a rotating disk in (12)CO(2-1) and (13)CO(2-1) emission and resolve the continuum emission at 1.3 mm. We infer disk gas and dust masses of similar to 110 and similar to 40 Earth masses, respectively. Fits to a power-law disk model indicate that the molecular disk extends to similar to 370 AU and is viewed at an inclination of between similar to 33 degrees and similar to 39 degrees for dynamical stellar masses ranging from 1.8 M(circle dot) down to 1.5 M(circle dot) (the range of the total mass previously determined for the central, 2.4 day spectroscopic binary). This range of disk inclination is consistent with that assumed in deducing the central binary mass (i.e., 35 degrees), suggesting that the V4046 Sgr binary system and its circumbinary, molecular disk are coplanar. In light of the system's age and binarity, the presence of an extensive molecular disk orbiting V4046 Sgr provides constraints on the timescales of processes related to Jovian planet formation and demonstrates that circumbinary Jovian planets potentially could form around close binary systems. C1 [Rodriguez, David R.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Kastner, Joel H.] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA. [Wilner, David; Qi, Chunhua] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Rodriguez, DR (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. EM drodrigu@astro.ucla.edu; jhk@cis.rit.edu; dwilner@cfa.harvard.edu; cqi@cfa.harvard.edu FU Smithsonian Institution; Academia Sinica; NASA [NNX09AC96G] FX We thank Ben Zuckerman for useful discussions and comments and Meredith Hughes for lending us her deprojected visibility code. We are grateful to Michiel Hogerheijde for providing access to the two-dimensional version of RATRAN used in this work. We appreciate the suggestions and comments of the anonymous referee. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. This research was supported by NASA Astrophysics Data Analysis Program grant NNX09AC96G to RIT and UCLA. NR 51 TC 31 Z9 31 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2010 VL 720 IS 2 BP 1684 EP 1690 DI 10.1088/0004-637X/720/2/1684 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647ND UT WOS:000281624300061 ER PT J AU Schwamb, ME Brown, ME Rabinowitz, DL Ragozzine, D AF Schwamb, Megan E. Brown, Michael E. Rabinowitz, David L. Ragozzine, Darin TI PROPERTIES OF THE DISTANT KUIPER BELT: RESULTS FROM THE PALOMAR DISTANT SOLAR SYSTEM SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE Kuiper Belt: general; Oort Cloud ID TRANS-NEPTUNIAN OBJECTS; EMBEDDED STAR-CLUSTERS; OORT CLOUD; CANDIDATE MEMBERS; SIZE DISTRIBUTION; STELLAR CLUSTERS; MOLECULAR CLOUDS; INFRARED IMAGES; SCATTERED DISK; PERIOD COMETS AB We present the results of a wide-field survey using the 1.2 m Samuel Oschin Telescope at Palomar Observatory. This survey was designed to find the most distant members of the Kuiper Belt and beyond. We searched similar to 12,000 deg(2) down to a mean limiting magnitude of 21.3 in R. A total number of 52 Kuiper Belt objects and Centaurs have been detected, 25 of which were discovered in this survey. Except for the redetection of Sedna, no additional Sedna-like bodies with perihelia greater than 45 AU were detected despite sensitivity out to distances of 1000 AU. We discuss the implications for a distant Sedna-like population beyond the Kuiper Belt, focusing on the constraints we can place on the embedded stellar cluster environment the early Sun may be have been born in, where the location and distribution of Sedna-like orbits sculpted by multiple stellar encounters is indicative of the birth cluster size. We also report our observed latitude distribution and implications for the size of the plutino population. C1 [Schwamb, Megan E.; Brown, Michael E.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Rabinowitz, David L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Ragozzine, Darin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schwamb, ME (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM mschwamb@gps.caltech.edu RI Ragozzine, Darin/C-4926-2013; OI Schwamb, Megan/0000-0003-4365-1455 FU NASA [NNG05GI02G] FX This research is supported by NASA Origins of Solar Systems Program grant NNG05GI02G. M. E. S. is supported by a NASA Earth and Space Science Fellowship. We are indebted to Ramon Brasser and Nathan Kaib for sharing the results of their cluster integrations and to J. J. Kavellaars, Brett Gladman, and Samantha Lawler for providing us with the nominal CFEPS plutino model. We thank the staff at Palomar Observatory for their dedicated support of the robotic operation of the Samuel Oschin Telescope and QUEST camera. The authors also thank Greg Aldering for his help in scheduling the observations. We acknowledge Mansi Kasliwal, Henry Roe, John Subasavage, Emily Schaller, and Richard Walters for their assistance with recovery observations of our new discoveries. We recognize the work of Christian Clanton for support in developing the dynamical integration tools. We also thank Wes Fraser, Ramon Brasser, and Nathan Kaib for insightful conversations. NR 79 TC 35 Z9 35 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2010 VL 720 IS 2 BP 1691 EP 1707 DI 10.1088/0004-637X/720/2/1691 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647ND UT WOS:000281624300062 ER PT J AU Lattanzi, V Gottlieb, CA Thaddeus, P Thorwirth, S McCarthy, MC AF Lattanzi, V. Gottlieb, C. A. Thaddeus, P. Thorwirth, S. McCarthy, M. C. TI THE ROTATIONAL SPECTRUM OF THE NCO- ANION SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (Sgr B2); ISM: molecules; line: identification; molecular data; molecular processes; radio lines: ISM ID NEGATIVE-IONS; ASTRONOMICAL IDENTIFICATION; AUTODETACHMENT SPECTROSCOPY; LASER SPECTROSCOPY; COUPLED-CLUSTER; INTERSTELLAR; ACID; HNCO; CN; DYNAMICS AB The rotational spectrum of the negative molecular ion NCO- has been observed both in a supersonic molecular beam and in a low-pressure glow discharge. The identification is ironclad because of the previous infrared detection of NCO-, the presence of well-resolved nitrogen quadrupole hyperfine structure, and the observation of nine harmonically related transitions in the millimeter band. The spectroscopic constants B and D are three orders of magnitude more accurate than those derived from the earlier IR measurements, and the theoretical eQq is in good agreement with that measured. The entire rotational spectrum can now be calculated well into the THz region to 1 km s(-1) in equivalent radial velocity or better. NCO- is an excellent candidate for radio astronomical detection because of its high stability, polarity, and favorable partition function. The fairly high concentration of NCO- in our laboratory source implies that other molecular anions containing the NCO group may be detectable in the radio band. C1 [Lattanzi, V.; Gottlieb, C. A.; Thaddeus, P.; McCarthy, M. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lattanzi, V.; Gottlieb, C. A.; Thaddeus, P.; McCarthy, M. C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Thorwirth, S.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Thorwirth, S.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Lattanzi, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM vlattanzi@cfa.harvard.edu; cgottlieb@cfa.harvard.edu; pthaddeus@cfa.harvard.edu; sthorwirth@ph1.uni-koeln.de; mccarthy@cfa.harvard.edu RI Thorwirth, Sven/C-6217-2011; OI Thorwirth, Sven/0000-0001-8200-6710; McCarthy, Michael/0000-0001-9142-0008 FU NSF [CHE-0701204]; NASA [NNX08AE05G]; Deutsche Forschungsgemeinschaft [TH 1301/3-1] FX It is a pleasure to acknowledge R. Saykally for illuminating discussions on the production and detection of ions in the laboratory. The authors thank V. Bierbaum, E. Herbst, and A. Viggiano for comments on ion chemistry, and K. Oberg on interstellar ices; and M. Guelin for helpful discussions on the astronomical observations of negative ions. The work in Cambridge is supported by the NSF grant CHE-0701204 and NASA grant NNX08AE05G. S. T. is grateful to the Deutsche Forschungsgemeinschaft for a research grant (TH 1301/3-1). NR 39 TC 12 Z9 12 U1 5 U2 11 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2010 VL 720 IS 2 BP 1717 EP 1720 DI 10.1088/0004-637X/720/2/1717 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647ND UT WOS:000281624300064 ER PT J AU Luhman, KL Mamajek, EE Allen, PR Muench, AA Finkbeiner, DP AF Luhman, K. L. Mamajek, E. E. Allen, P. R. Muench, A. A. Finkbeiner, D. P. TI DISCOVERY OF A WIDE BINARY BROWN DWARF BORN IN ISOLATION (vol 691, pg 1265, 2009) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Luhman, K. L.; Allen, P. R.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Mamajek, E. E.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Muench, A. A.; Finkbeiner, D. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Luhman, KL (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM kluhman@astro.psu.edu NR 7 TC 3 Z9 3 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2010 VL 720 IS 2 BP 1781 EP 1781 DI 10.1088/0004-637X/720/2/1781 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647ND UT WOS:000281624300071 ER PT J AU Drake, JJ Orlando, S AF Drake, J. J. Orlando, S. TI THE EARLY BLAST WAVE OF THE 2010 EXPLOSION OF U SCORPII SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE methods: numerical; novae, cataclysmic variables; shock waves; stars: individual (U Sco); X-rays: binaries ID NOVA RS-OPHIUCHI; X-RAY-EMISSION; 2006 OUTBURST; RECURRENT NOVAE; SUPERNOVA-REMNANTS; WHITE-DWARF; SPECTROSCOPY; HYDRODYNAMICS; SIMULATIONS; ACCRETION AB Three-dimensional hydrodynamic simulations exploring the first 18 hr of the 2010 January 28 outburst of the recurrent nova U Scorpii have been performed. Special emphasis was placed on capturing the enormous range in spatial scales in the blast. The pre-explosion system conditions included the secondary star and a flared accretion disk. These conditions can have a profound influence on the evolving blast wave. The blast itself is shadowed by the secondary star, which itself gives rise to a low-temperature bow shock. The accretion disk is completely destroyed in the explosion. A model with a disk gas density of 10(15) cm(-3) produced a blast wave that is collimated and with clear bipolar structures, including a bipolar X-ray emitting shell. The degree of collimation depends on the initial mass of ejecta, energy of explosion, and circumstellar gas density distribution. It is most pronounced for a model with the lowest explosion energy (10(43) erg) and mass of ejecta (10(-8) M(circle dot)). The X-ray luminosities of three of six models computed are close to, but consistent with, an upper limit to the early blast X-ray emission obtained by the Swift satellite, the X-ray luminosity being larger for higher circumstellar gas density and higher ejecta mass. The latter consideration, together with estimates of the blast energy from previous outbursts, suggests that the mass of ejecta in the 2010 outburst was not larger than 10(-7) M(circle dot). C1 [Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Orlando, S.] INAF Osservatorio Astron Palermo GS Vaiana, I-90134 Palermo, Italy. RP Drake, JJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Orlando, Salvatore/0000-0003-2836-540X FU NASA [NAS8-39073]; DOE FX J.J.D. was funded by NASA contract NAS8-39073 to the Chandra X-ray Center. FLASH was developed by the DOE-supported ASC/Alliance Center for Astrophysical Thermonuclear Flashes, University of Chicago. Simulations were executed at the HPC SCAN facility of INAF-OAPA. NR 47 TC 19 Z9 19 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 10 PY 2010 VL 720 IS 2 BP L195 EP L200 DI 10.1088/2041-8205/720/2/L195 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647HX UT WOS:000281610200014 ER PT J AU Magdis, GE Elbaz, D Hwang, HS Daddi, E Rigopoulou, D Altieri, B Andreani, P Aussel, H Berta, S Cava, A Bongiovanni, A Cepa, J Cimatti, A Dickinson, M Dominguez, H Schreiber, NF Genzel, R Huang, JS Lutz, D Maiolino, R Magnelli, B Morrison, GE Nordon, R Garcia, AMP Poglitsch, A Popesso, P Pozzi, F Riguccini, L Rodighiero, G Saintonge, A Santini, P Sanchez-Portal, M Shao, L Sturm, E Tacconi, L Valtchanov, I AF Magdis, G. E. Elbaz, D. Hwang, H. S. Daddi, E. Rigopoulou, D. Altieri, B. Andreani, P. Aussel, H. Berta, S. Cava, A. Bongiovanni, A. Cepa, J. Cimatti, A. Dickinson, M. Dominguez, H. Schreiber, N. Foerster Genzel, R. Huang, J. -S. Lutz, D. Maiolino, R. Magnelli, B. Morrison, G. E. Nordon, R. Garcia, A. M. Perez Poglitsch, A. Popesso, P. Pozzi, F. Riguccini, L. Rodighiero, G. Saintonge, A. Santini, P. Sanchez-Portal, M. Shao, L. Sturm, E. Tacconi, L. Valtchanov, I. TI A FIRST GLIMPSE INTO THE FAR-IR PROPERTIES OF HIGH-z UV-SELECTED GALAXIES: HERSCHEL/PACS OBSERVATIONS OF z similar to 3 LBGS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmology: observations; galaxies: evolution; galaxies: formation; galaxies: general; galaxies: high-redshift; infrared: galaxies ID LYMAN-BREAK GALAXIES; ULTRALUMINOUS INFRARED GALAXIES; STAR-FORMATION; STELLAR MASSES; DUST; MULTIWAVELENGTH; Z-SIMILAR-TO-3; POPULATION; SPECTRA AB We present first insights into the far-IR properties for a sample of IRAC and MIPS 24 mu m detected Lyman break galaxies (LBGs) at z similar to 3, as derived from observations in the northern field of the Great Observatories Origins Survey (GOODS-N) carried out with the PACS instrument on board the Herschel Space Observatory. Although none of our galaxies are detected by Herschel, we employ a stacking technique to construct, for the first time, the average spectral energy distribution (SED) of infrared luminous LBGs from UV to radio wavelengths. We derive a median IR luminosity of L(IR) = 1.6 x 10(12) L(circle dot), placing the population in the class of ultra-luminous infrared galaxies (ULIRGs). Complementing our study with existing multi-wavelength data, we put constraints on the dust temperature of the population and find that for their L(IR), MIPS-LBGs are warmer than submillimeter-luminous galaxies while they fall in the locus of the L(IR)-T(d) relation of the local ULIRGs. This, along with estimates based on the average SED, explains the marginal detection of LBGs in current submillimeter surveys and suggests that these latter studies introduce a bias toward the detection of colder ULIRGs in the high-z universe, while missing high-z ULIRGS with warmer dust. C1 [Magdis, G. E.; Elbaz, D.; Hwang, H. S.; Daddi, E.; Aussel, H.; Riguccini, L.] CEA, Lab AIM, Irfu SAp, F-91191 Gif Sur Yvette, France. [Rigopoulou, D.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. European Space Astron Ctr, Villafrance del Castillo, Spain. [Andreani, P.] ESO, D-85748 Garching, Germany. [Berta, S.; Schreiber, N. Foerster; Genzel, R.; Lutz, D.; Magnelli, B.; Nordon, R.; Poglitsch, A.; Popesso, P.; Saintonge, A.; Sanchez-Portal, M.; Shao, L.; Sturm, E.; Tacconi, L.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. [Cava, A.; Bongiovanni, A.; Cepa, J.; Garcia, A. M. Perez] Inst Astrofis Canarias, San Cristobal la Laguna 38205, Spain. [Cimatti, A.; Rodighiero, G.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Dickinson, M.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Dominguez, H.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Huang, J. -S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Maiolino, R.; Pozzi, F.; Santini, P.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Morrison, G. E.] Univ Hawaii, Inst Astron, Honolulu, HI USA. [Morrison, G. E.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, Villafranca Castillo Satellite Tracking Stn, Madrid, Spain. RP Magdis, GE (reprint author), CEA, Lab AIM, Irfu SAp, F-91191 Gif Sur Yvette, France. RI Daddi, Emanuele/D-1649-2012; Magdis, Georgios/C-7295-2014; Bongiovanni, Angel/J-6176-2012; Cava, Antonio/C-5274-2017; OI Daddi, Emanuele/0000-0002-3331-9590; Magdis, Georgios/0000-0002-4872-2294; Cava, Antonio/0000-0002-4821-1275; Santini, Paola/0000-0002-9334-8705; Altieri, Bruno/0000-0003-3936-0284 FU BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI (Italy); CICT/MCT (Spain) FX PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KUL, CSL, IMEC (Belgium); CEA, OAMP (France); MPIA (Germany); IFSI, OAP/AOT, OAA/CAISMI, LENS, SISSA (Italy); and IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI (Italy), and CICT/MCT (Spain). NR 33 TC 30 Z9 30 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 10 PY 2010 VL 720 IS 2 BP L185 EP L189 DI 10.1088/2041-8205/720/2/L185 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647HX UT WOS:000281610200012 ER PT J AU Matranga, M Drake, JJ Kashyap, VL Marengo, M Kuchner, MJ AF Matranga, M. Drake, J. J. Kashyap, V. L. Marengo, M. Kuchner, M. J. TI CLOSE BINARIES WITH INFRARED EXCESS: DESTROYERS OF WORLDS? SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: close; circumstellar matter; infrared: stars; stars: individual (AR Psc, II Peg, UX Ari) ID RS CANUM-VENATICORUM; SUN-LIKE; DEBRIS DISKS; PHOTOMETRIC-OBSERVATIONS; RESONANT SIGNATURES; PLANETARY SYSTEMS; ACTIVE STARS; SPITZER MIPS; WARM DUST; II PEGASI AB We present the results of a Spitzer photometric investigation into the IR excesses of close binary systems. In a sample of 10 objects, excesses in Infrared Array Camera and MIPS24 bands implying the presence of warm dust are found for 3. For two objects, we do not find excesses reported in earlier IRAS studies. We discuss the results in the context of the scenario suggested by Rhee and co-workers, in which warm dust is continuously created by destructive collisions between planetary bodies. A simple numerical model for the steady-state distribution of dust in one IR excess system shows a central clearing of radius 0.22 AU caused by dynamical perturbations from the binary star. This is consistent with the size of the central clearing derived from the Spitzer spectral energy distribution. We conclude that close binaries could be efficient "destroyers of worlds" and lead to destabilization of the orbits of their planetary progeny by magnetically driven angular momentum loss and secular shrinkage of the binary separation. C1 [Matranga, M.; Drake, J. J.; Kashyap, V. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marengo, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kuchner, M. J.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab Greenbelt, Greenbelt, MD 20771 USA. RP Matranga, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Kuchner, Marc/E-2288-2012 FU Spitzer [1279130]; NASA [NAS8-39073, 1407] FX M. Matranga was supported by Spitzer contract 1279130. J.J.D. and V. L. K. were funded by the NASA contract NAS8-39073 to the Chandra X-ray Center. Observations were made with Spitzer, operated by JPL under the NASA contract 1407. NR 47 TC 5 Z9 6 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 10 PY 2010 VL 720 IS 2 BP L164 EP L168 DI 10.1088/2041-8205/720/2/L164 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647HX UT WOS:000281610200008 ER PT J AU Mueller, UG Scott, JJ Ishak, HD Cooper, M Rodrigues, A AF Mueller, Ulrich G. Scott, Jarrod J. Ishak, Heather D. Cooper, Michael Rodrigues, Andre TI Monoculture of Leafcutter Ant Gardens SO PLOS ONE LA English DT Article ID FUNGUS-GROWING ANTS; LEAF-CUTTER ANTS; ATTINE ANT; DISEASE MANAGEMENT; SYMBIONT CHOICE; ATTA-SEXDENS; EVOLUTION; FORMICIDAE; COOPERATION; CONFLICT AB Background: Leafcutter ants depend on the cultivation of symbiotic Attamyces fungi for food, which are thought to be grown by the ants in single-strain, clonal monoculture throughout the hundreds to thousands of gardens within a leafcutter nest. Monoculture eliminates cultivar-cultivar competition that would select for competitive fungal traits that are detrimental to the ants, whereas polyculture of several fungi could increase nutritional diversity and disease resistance of genetically variable gardens. Methodology/Principal Findings: Using three experimental approaches, we assessed cultivar diversity within nests of Atta leafcutter ants, which are most likely among all fungus-growing ants to cultivate distinct cultivar genotypes per nest because of the nests' enormous sizes (up to 5000 gardens) and extended lifespans (10-20 years). In Atta texana and in A. cephalotes, we resampled nests over a 5-year period to test for persistence of resident cultivar genotypes within each nest, and we tested for genetic differences between fungi from different nest sectors accessed through excavation. In A. texana, we also determined the number of Attamyces cells carried as a starter inoculum by a dispersing queens (minimally several thousand Attamyces cells), and we tested for genetic differences between Attamyces carried by sister queens dispersing from the same nest. Except for mutational variation arising during clonal Attamyces propagation, DNA fingerprinting revealed no evidence for fungal polyculture and no genotype turnover during the 5-year surveys. Conclusions/Significance: Atta leafcutter ants can achieve stable, fungal monoculture over many years. Mutational variation emerging within an Attamyces monoculture could provide genetic diversity for symbiont choice (gardening biases of the ants favoring specific mutational variants), an analog of artificial selection. C1 [Mueller, Ulrich G.; Scott, Jarrod J.; Ishak, Heather D.; Cooper, Michael; Rodrigues, Andre] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Mueller, Ulrich G.; Scott, Jarrod J.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Scott, Jarrod J.] Univ Wisconsin, Dept Bacteriol, Madison, WI 53706 USA. [Rodrigues, Andre] State Univ Sao Paulo UNESP, Ctr Study Social Insects, Sao Paulo, Brazil. [Rodrigues, Andre] Santa Cruz State Univ UESC, Dept Biol Sci, Ilheus, BA, Brazil. RP Mueller, UG (reprint author), Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. EM umueller@mail.utexas.edu RI Rodrigues, Andre/B-8148-2012 OI Rodrigues, Andre/0000-0002-4164-9362 FU National Science Foundation [DEB-0920138, DEB-0639879, DEB-0110073, DEB-0949689]; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico [02/05] FX The research was supported by National Science Foundation awards DEB-0920138, DEB-0639879, and DEB-0110073 to UGM; DEB-0949689 to T. R. Schultz, N. Mehdiabadi, and UGM; and a Fellowship (02/05) from the Conselho Nacional de Desenvolvimento Cientifico e Tecnologico to AR. The funding agencies had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 71 TC 18 Z9 18 U1 3 U2 23 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD SEP 10 PY 2010 VL 5 IS 9 AR e12668 DI 10.1371/journal.pone.0012668 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 648IX UT WOS:000281687300012 ER PT J AU Onofrio, R AF Onofrio, Roberto TI Higgs-induced spectroscopic shifts near strong gravity sources SO PHYSICAL REVIEW D LA English DT Article ID GALACTIC-CENTER REGION; SAGITTARIUS A-ASTERISK; ENERGY-MOMENTUM TENSOR; GAUGE FIELD-THEORIES; BLACK-HOLE; MASSLESS PARTICLES; MOLECULAR CLOUD; CARBON-MONOXIDE; PROPER-MOTION; GALAXY AB We explore the consequences of the mass generation due to the Higgs field in strong gravity astrophysical environments. The vacuum expectation value of the Higgs field is predicted to depend on the curvature of spacetime, potentially giving rise to peculiar spectroscopic shifts, named hereafter "Higgs shifts." Higgs shifts could be searched through dedicated multiwavelength and multispecies surveys with high spatial and spectral resolution near strong gravity sources such as Sagittarius A* or broad searches for signals due to primordial black holes. The possible absence of Higgs shifts in these surveys should provide limits to the coupling between the Higgs particle and the curvature of spacetime, a topic of interest for a recently proposed Higgs-driven inflationary model. We discuss some conceptual issues regarding the coexistence between the Higgs mechanism and gravity, especially for their different handling of fundamental and composite particles. C1 [Onofrio, Roberto] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy. [Onofrio, Roberto] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Onofrio, R (reprint author), Univ Padua, Dipartimento Fis G Galilei, Via Marzolo 8, I-35131 Padua, Italy. EM onofrior@gmail.com FU Julian Schwinger Foundation [JSF 08070000] FX We are grateful to F. de Felice for fruitful discussions, and H. R. Sadeghpour and L. Viola for a critical reading of the manuscript. Partial support from the Julian Schwinger Foundation through grant JSF 08070000 on Astrophysics of Quantum Vacuum is also acknowledged. NR 51 TC 9 Z9 9 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD SEP 9 PY 2010 VL 82 IS 6 AR 065008 DI 10.1103/PhysRevD.82.065008 PG 5 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 647ZI UT WOS:000281659000004 ER PT J AU O'Byrne, G Martin, RV van Donkelaar, A Joiner, J Celarier, EA AF O'Byrne, G. Martin, R. V. van Donkelaar, A. Joiner, J. Celarier, E. A. TI Surface reflectivity from the Ozone Monitoring Instrument using the Moderate Resolution Imaging Spectroradiometer to eliminate clouds: Effects of snow on ultraviolet and visible trace gas retrievals SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID NORTHERN-HEMISPHERE; SPECTRAL ALBEDO; GOME MEASUREMENTS; TROPOSPHERIC NO2; COVERED SURFACES; MODIS; PRODUCTS; SPACE; UV; ALGORITHM AB Satellite retrievals of tropospheric composition from measurements of solar backscatter require accurate information about surface reflectivity. We use clear-sky data from the Ozone Monitoring Instrument (OMI) to determine global surface reflectivity under both snow-covered and snow-free conditions at 354 nm. Clear-sky scenes are determined using cloud and aerosol data from the Moderate Resolution Imaging Spectroradiometer/Aqua satellite instrument that flies 12 min ahead of OMI/Aura. The result is a database of OMI-observed Lambertian equivalent reflectivity (LER) that does not rely on statistical methods to eliminate cloud and aerosol contamination. We apply this database to evaluate previous climatologies of surface reflectivity. Except for regions of seasonal snow cover, agreement is best with a climatology from OMI, which selects the surface reflectivity from a histogram of observed LER (mean difference, 0.0002; standard deviation, 0.011). Three other climatologies of surface reflectivity from Total Ozone Mapping Spectrometer, Global Ozone Monitoring Experiment, and OMI, based on minimum observed LER, are less consistent with our cloud-and aerosol-filtered data set (mean difference, -0.008, 0.012, and -0.002; standard deviation, 0.022, 0.026, and 0.033). Snow increases the sensitivity of solar backscatter measurements at ultraviolet and visible wavelengths to trace gases in the lower troposphere. However, all four existing LER climatologies poorly represent seasonal snow. Surface reflectivity over snow-covered lands depends strongly on the vegetation type covering the surface. The monthly variation of snow-covered reflectivity varies by less than 0.1 in fall and winter. Applying our snow-covered surface reflectivity database to OMI NO2 retrievals could change the retrieved NO2 column by 20%-50% over large regions with seasonal snow cover. C1 [O'Byrne, G.; Martin, R. V.; van Donkelaar, A.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. [Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Joiner, J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Celarier, E. A.] Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP O'Byrne, G (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. EM randall.martin@dal.ca RI Joiner, Joanna/D-6264-2012; Martin, Randall/C-1205-2014 OI Martin, Randall/0000-0003-2632-8402 FU NASA; Canadian Foundation for Climate and Atmospheric Science FX Terry O'Byrne and two anonymous reviewers provided helpful comments that improved this manuscript. We thank the OMI and MODIS teams as well as Environment Canada for making their data publicly available. This research was supported by NASA and the Canadian Foundation for Climate and Atmospheric Science. NR 57 TC 10 Z9 10 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD SEP 8 PY 2010 VL 115 AR D17305 DI 10.1029/2009JD013079 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 649GF UT WOS:000281755400002 ER PT J AU Chesser, RT Yeung, CKL Yao, CT Tian, XH Li, SH AF Chesser, R. Terry Yeung, Carol K. L. Yao, Cheng-Te Tian, Xiu-Hua Li, Shou-Hsien TI Molecular phylogeny of the spoonbills (Aves: Threskiornithidae) based on mitochondrial DNA SO ZOOTAXA LA English DT Article DE spoonbills; Platalea; Threskiornithidae; mitochondrial DNA ID LIKELIHOOD; ACCURATE; MODELS; BIRDS AB Spoonbills (genus Platalea) are a small group of wading birds, generally considered to constitute the subfamily Plataleinae (Aves: Threskiornithidae). We reconstructed phylogenetic relationships among the six species of spoonbills using variation in sequences of the mitochondrial genes ND2 and cytochrome b (total 1796 bp). Topologies of phylogenetic trees reconstructed using maximum likelihood, maximum parsimony, and Bayesian analyses were virtually identical and supported monophyly of the spoonbills. Most relationships within Platalea received strong support: P. minor and P. regia were closely related sister species, P. leucorodia was sister to the minor-regia clade, and P. alba was sister to the minor-regia-leucorodia clade. Relationships of P. flavipes and P. ajaja were less well resolved: these species either formed a clade that was sister to the four-species clade, or were successive sisters to this clade. This phylogeny is consistent with ideas of relatedness derived from spoonbill morphology. Our limited sampling of the Threskiornithinae (ibises), the putative sister group to the spoonbills, indicated that this group is paraphyletic, in agreement with previous molecular data; this suggests that separation of the Threskiornithidae into subfamilies Plataleinae and Threskiornithinae may not be warranted. C1 [Chesser, R. Terry] Smithsonian Inst, Natl Museum Nat Hist, Patuxent Wildlife Res Ctr, US Geol Survey, Washington, DC 20560 USA. [Yeung, Carol K. L.; Li, Shou-Hsien] Natl Taiwan Normal Univ, Dept Life Sci, Taipei 11677, Taiwan. [Yao, Cheng-Te] Endem Species Res Inst, Chi Chi 552, Nantou, Taiwan. [Yao, Cheng-Te] Natl Cheng Kung Univ, Dept Life Sci, Tainan 701, Taiwan. [Tian, Xiu-Hua] NE Forestry Univ, Coll Wildlife, Harbin 150040, Peoples R China. RP Chesser, RT (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Patuxent Wildlife Res Ctr, US Geol Survey, Washington, DC 20560 USA. FU National Science Council, Taiwan, R.O.C. FX We thank the American Museum of Natural History, New York, and the Australian National Wildlife Collection, Canberra, for providing samples, and two anonymous reviewers for comments on the manuscript. This work was supported by grants to S.-H.L. from the National Science Council, Taiwan, R.O.C. Use of trade, product, or firm names does not imply endorsement by the U.S. Government. NR 23 TC 8 Z9 8 U1 3 U2 8 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD SEP 6 PY 2010 IS 2603 BP 53 EP 60 PG 8 WC Zoology SC Zoology GA 646GD UT WOS:000281525600002 ER PT J AU Murphy, NA Sovinec, CR Cassak, PA AF Murphy, N. A. Sovinec, C. R. Cassak, P. A. TI Magnetic reconnection with asymmetry in the outflow direction SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID CORONAL MASS EJECTION; TIME-DEPENDENT RECONNECTION; DRIVEN STELLAR WINDS; CME CURRENT SHEETS; X-LINE; DENSITY ASYMMETRY; GEOMAGNETIC TAIL; MHD SIMULATIONS; ACTIVE-REGION; SOLAR-FLARES AB Magnetic reconnection with asymmetry in the outflow direction occurs in the Earth's magnetotail, coronal mass ejections, flux cancellation events, astrophysical disks, spheromak merging experiments, and elsewhere in nature and the laboratory. A control volume analysis is performed for the case of steady antiparallel magnetic reconnection with asymmetric downstream pressure to derive scaling relations for the outflow velocity from each side of the current sheet and the reconnection rate. Simple relationships for outflow velocity are presented for the incompressible case and the case of symmetric downstream pressure but asymmetric downstream density. Asymmetry alone is not found to greatly affect the reconnection rate. The flow stagnation point and magnetic field null do not coincide in a steady state unless the pressure gradient is negligible at the flow stagnation point. The predictions of the model are compared with resistive MHD simulations of driven reconnection with asymmetry in the outflow direction. C1 [Murphy, N. A.; Sovinec, C. R.] Univ Wisconsin, Ctr Magnet Self Org Lab & Astrophys Plasmas, Madison, WI 53706 USA. [Murphy, N. A.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Sovinec, C. R.] Univ Wisconsin, Dept Engn Phys, Madison, WI 53706 USA. [Cassak, P. A.] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA. RP Murphy, NA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 16, Cambridge, MA 02138 USA. EM namurphy@cfa.harvard.edu OI Murphy, Nicholas/0000-0001-6628-8033 FU NSF, through the Center for Magnetic Self-Organization in Laboratory and Astrophysical Plasmas [PHY-0821899]; NASA [NNX09AB17G]; NSF [PHY-0902479] FX The authors thank Ellen Zweibel, Jennifer Stone, Michiaki Inomoto, John Raymond, Ping Zhu, Yi-Min Huang, Michael Shay, Clare Parnell, Dmitri Uzdensky, Mitsuo Oka, Joseph Cassinelli, Richard Townsend, K. Tabetha Hole, John Everett, Seth Dorfman, and Samuel Friedman for useful discussions. N. A. M. and C. R. S. acknowledge support from NSF grant PHY-0821899 through the Center for Magnetic Self-Organization in Laboratory and Astrophysical Plasmas. N. A. M. acknowledges additional support from NASA grant NNX09AB17G to the Smithsonian Astrophysical Observatory. P. A. C. acknowledges support from NSF grant PHY-0902479. This research has benefited from use of NASA's Astrophysics Data System Bibliographic Services. NR 95 TC 21 Z9 21 U1 1 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD SEP 4 PY 2010 VL 115 AR A09206 DI 10.1029/2009JA015183 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647QM UT WOS:000281633700003 ER PT J AU Zatwarnicki, T Mathis, WN AF Zatwarnicki, Tadeusz Mathis, Wayne N. TI A Revision of the nivea Group of the Shore-fly Genus Ditrichophora Cresson (Diptera: Ephydridae) SO TRANSACTIONS OF THE AMERICAN ENTOMOLOGICAL SOCIETY LA English DT Article DE Revision; Diptera; Ephydridae; shore flies; Ditrichophora; Holarctic Region AB Species of the nivea group (genus Ditrichophora Cresson) are revised. The group now includes four species of which one, D. gulkana (Alaska and Mongolia), is newly described. The group is now known to have a Holarctic distribution with two species, D. gulkana and D. nivea, being the first reported from the Nearctic Region. Another Asian species, D. brunnicosa, previously placed in Diclasiopa, is transferred to this group (genus Ditrichophora) and is also reported from Mongolia. To facilitate identification of these rare species, we have included diagnoses of the tribe, genus, and species group and have also provided an annotated key to Holarctic genera of the tribe Discocerinini and to species of the nivea group within Ditrichophora. We also provide the first illustrations of male terminalia for all included species. C1 [Zatwarnicki, Tadeusz] Opole Univ, Dept Biosystemat, PL-45052 Opole, Poland. [Mathis, Wayne N.] Dept Entomol, Washington, DC 20013 USA. Smithsonian Inst, Washington, DC 20013 USA. RP Zatwarnicki, T (reprint author), Opole Univ, Dept Biosystemat, Ul Oleska 22, PL-45052 Opole, Poland. EM zatwar@uni.opole.pl; mathisw@si.edu OI Zatwarnicki, Tadeusz/0000-0003-2163-0143 FU Altai and Hangai Mountains' drainages, Mongolia; United States National Science Foundation [DEB-0743732] FX Field work in Mongolia was generously supported by a grant entitled "Survey and Inventory of the Aquatic Insects of the Altai and Hangai Mountains' drainages, Mongolia" awarded to J. Gelhaus, J. Morse, C. R. Nelson. United States National Science Foundation: Biodiversity Inventories Program (DEB-0743732), awarded for 2008-2011. We are especially indebted to the principal investigators, Jon K. Gelhaus in particular, for inviting us to participate in the program and field work in the summer of 2009. NR 28 TC 0 Z9 0 U1 0 U2 1 PU AMER ENTOMOL SOC PI PHILADELPHIA PA 1900 BENJ FRANKLIN PARKWAY, PHILADELPHIA, PA 19103-1195 USA SN 0002-8320 J9 T AM ENTOMOL SOC JI Trans. Am. Entomol. Soc. PD SEP-DEC PY 2010 VL 136 IS 3-4 BP 199 EP 215 PG 17 WC Entomology SC Entomology GA 716EF UT WOS:000286951200001 ER PT J AU Fornshell, JA Tesei, A Fox, PD AF Fornshell, John A. Tesei, Alessandra Fox, Paul D. TI Acoustic Signatures of Three Marine Arthropods, Squilla mantis (Linnaeus, 1758), Homarus americanus (H. Milne Edwards, 1837), and Nephrops norvegicus (Linnaeus, 1758) (Arthropoda, Malacostraca) SO MARINE TECHNOLOGY SOCIETY JOURNAL LA English DT Article ID ZOOPLANKTON GROUPS; SOUND-SCATTERING; LOBSTER; MECHANISMS AB The acoustic signatures of three marine crustaceans, Squilla mantis (Linnaeus, 1758), Homarus americanus (H. Milne Edwards, 1837), and Nephrops norvegicus (Linnaeus 1758) (Arthropoda, Malacostraca), were experimetally determined in measurements using the calibration tank at the NATO Undersea Research Center, Le Spezia, Italy. The specimens were insonified at 45 rotational intervals with a sound source emitting pings from 30 to 120 kHz. For all three species, the value of the nondimensional parameter ka (where k is the acoustic wave number and a is the characteristic dimension of the object) was 5. The absorption specta, defined as the frequencies at which the intensity of the reflected sound was less than 5% of the incident intensity, were determined. These sepctra changed with the changing aspects and were unique for each animal in this study. Two of the species were in the same infraorder. Astacidea, Our reults contribute to the development of an acoustic identification system for surveys of marine animals. C1 [Fornshell, John A.] Smithsonian Inst, NATO Undersea Res Ctr NURC, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. [Tesei, Alessandra; Fox, Paul D.] Univ Southampton, Inst Sound & Vibrat Res, Southampton, Hants, England. RP Fornshell, JA (reprint author), Smithsonian Inst, NATO Undersea Res Ctr NURC, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. EM johnfornshell@hotmail.com FU NATO Undersea Research Centre (Italy) FX The NATO Undersea Research Centre (Italy) is gratefully acknowledged for having hosted John Fornshell and Paul Fox as Visiting Scientists during the period of the experimental work undertaken under the NURC Visiting Researchers Program 2009 and for providing all related facilities, support, and finance during that period. The Smithsonian Institution (USA) and the Institute of Sound and Vibration Research (UK) are also thanked for their affiliated support during the completion of the work. NR 28 TC 0 Z9 0 U1 0 U2 3 PU MARINE TECHNOLOGY SOC INC PI COLUMBIA PA 5565 STERRETT PLACE, STE 108, COLUMBIA, MD 21044 USA SN 0025-3324 J9 MAR TECHNOL SOC J JI Mar. Technol. Soc. J. PD SEP-OCT PY 2010 VL 44 IS 5 BP 67 EP 80 PG 14 WC Engineering, Ocean; Oceanography SC Engineering; Oceanography GA 679TP UT WOS:000284184000008 ER PT J AU Mawdsley, JR Sithole, H AF Mawdsley, Jonathan R. Sithole, Hendrik TI Diversity and abundance of insect visitors to flowers of trees and shrubs in a South African savannah SO AFRICAN JOURNAL OF ECOLOGY LA English DT Article DE landscape ecology; pollination; savannah; South Africa ID ACACIA-NIGRESCENS; POLLINATION; FABACEAE AB This study presents the results of a landscape-scale survey for insect floral visitors in the Skukuza Ranger District, Kruger National Park, South Africa. Floral visitors were sampled from flowering trees and shrubs along linear transects spanning the entire district. Six plant species were sampled in the late dry season (Acacia grandicornuta Gerstner, A. nigrescens Oliver, Cassia abbreviata Oliver, Combretum hereroense Schinz, Combretum zeyheri Sonder, Euclea divonorum Hiern), and eleven plant species were sampled during the rainy season (Acacia exuvialis Verdcourt, A. grandicornuta Gerstner, A. nilotica (L.) Willdenow, A. tortilis (Forsskal) Hayne, Dichrostachys cinerea Miquel, Flueggea virosa (Roxburgh) Baillon, Grewia bicolor Jussieu, G. flava De Candolle, G. flavescens Jussieu, G. monticola Sonder, and Peltophorum africanum Sonder). Coleoptera, Hymenoptera and Lepidoptera comprised the majority of floral visitors, while species of Blattodea, Diptera, Hemiptera and Neuroptera also occurred on flowers. Known or likely pollinators include bees (Hymenoptera: Apidae, Halictidae and Megachilidae) and scarab beetles (Coleoptera: Scarabaeidae). These plant species appear to have generalist pollination systems, with the exception of species of Grewia L., which appear to be pollinated primarily by bees. A provisional plant-pollinator food web is presented for the eleven species of trees and shrubs which flower during the rainy season.Resume Cet article presente les resultats d'une etude, realisee a l'echelle du paysage, des insectes qui visitent les fleurs dans le Skukuza Ranger District, dans le Parc National Kruger, en Afrique du Sud. Les insectes butineurs ont ete preleves dans des arbres et des arbustes en fleurs le long de transects lineaires qui traversent tout le district. On a echantillonne six especes vegetales en fin de saison seche (Acacia grandicornuta Gerstner, A. nigrescens Oliver, Cassia abbreviata Oliver, Combretum hereroense Schinz, Combretum zeyheri Sonder et Euclea divonorum Hiern), et 11 pendant la saison des pluies (Acacia exuvialis Verdcourt, A. grandicornuta Gerstner, A. nilotica (L.) Willdenow, A. tortilis (Forsskal) Hayne, Dichrostachys cinerea Miquel, Flueggea virosa (Roxburgh) Baillon, Grewia bicolor Jussieu, G. flava De Candolle, G. flavescens Jussieu, G. monticola Sonder, et Peltophorum africanum Sonder). Coleopteres, hymenopteres et lepidopteres composaient la majorite des insectes qui visitaient les fleurs et l'on voyait aussi sur les fleurs des especes de blattodees, de dipteres, d'hemipteres et de neuropteres. Les pollinisateurs connus ou supposes incluent des abeilles (Hymenopteres : Apides, Halictides et Megachilides) et des scarabees (Coleopteres : Scarabeides). Ces especes vegetales semblent avoir des systemes de pollinisation generalistes, a l'exception d'especes de Grewia L. qui semblent etre fertilises d'abord par les abeilles. Un reseau alimentaire provisoire plantes-pollinisateurs est presente pour les 11 especes d'arbres et d'arbustes qui fleurissent pendant la saison des pluies. C1 [Mawdsley, Jonathan R.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, MRC 187, Washington, DC 20013 USA. [Sithole, Hendrik] Kruger Natl Pk, ZA-1350 Skukuza, South Africa. RP Mawdsley, JR (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, MRC 187, POB 37012, Washington, DC 20013 USA. EM mawdsley@heinzctr.org NR 21 TC 4 Z9 4 U1 2 U2 23 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0141-6707 J9 AFR J ECOL JI Afr. J. Ecol. PD SEP PY 2010 VL 48 IS 3 BP 691 EP 698 DI 10.1111/j.1365-2028.2009.01166.x PG 8 WC Ecology SC Environmental Sciences & Ecology GA 634WV UT WOS:000280617600014 ER PT J AU Arnoldi, MJ AF Arnoldi, Mary Jo TI Surfaces: Color, Substances, and Ritual Applications on African Sculpture SO AFRICAN STUDIES REVIEW LA English DT Book Review C1 [Arnoldi, Mary Jo] Smithsonian Inst, Washington, DC 20560 USA. RP Arnoldi, MJ (reprint author), Smithsonian Inst, Washington, DC 20560 USA. EM arnoldim@si.edu NR 1 TC 0 Z9 0 U1 0 U2 0 PU AFRICAN STUDIES REVIEW PI NEW BRUNSWICK PA RUTGERS, THE STATE UNIV NEW JERSEY, DOUGLAS CAMPUS, 132 GEORGE ST, NEW BRUNSWICK, NJ 08901-1400 USA SN 0002-0206 J9 AFR STUD REV JI Afr. Stud. Rev. PD SEP PY 2010 VL 53 IS 2 BP 221 EP 222 PG 2 WC Area Studies SC Area Studies GA 654HZ UT WOS:000282160400036 ER PT J AU Peterson, PM Romaschenko, K Johnson, G AF Peterson, Paul M. Romaschenko, Konstantin Johnson, Gabriel TI A PHYLOGENY AND CLASSIFICATION OF THE MUHLENBERGIINAE (POACEAE: CHLORIDOIDEAE: CYNODONTEAE) BASED ON PLASTID AND NUCLEAR DNA SEQUENCES SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE biogeography; Chloridoideae; classification; ITS; Muhlenbergia; Muhlenbergiinae; phylogeny; plastid DNA sequences; Poaceae ID C-4 GRASSES; NORTH; EVOLUTION; ERAGROSTIDEAE; PLANTS; DISJUNCTIONS; GRAMINEAE; TORTOISE; AMERICA; ANATOMY AB Premise of the study : To understand the origins of C(4) grasslands, we must have a better interpretation of plant traits via phylogenetic reconstruction. Muhlenbergiinae, the largest subtribe of C(4) grasses in Mexico and the southwestern United States (with 176 species), is taxonomically poorly understood. Methods : We conducted a phylogenetic analysis of 47 genera and 174 species using six plastid regions (ndhA intron, ndhF, rps16-trnK, rps16 intron, rps3, and rpl32-trnL) and the nuclear ITS 1 and 2 (ribosomal internal transcribed spacer) regions to infer evolutionary relationships and revise the classification. Key results : In our analyses, Muhlenbergia (ca. 153 species) is paraphyletic, with nine genera (Aegopogon, Bealia, Blepharoneuron, Chaboissaea, Lycurus, Muhlenbergia, Pereilema, Redfieldia, Schaffnerella, and Schedonnardus) found nested within. We recognized the following five well-supported monophyletic lineages within Muhlenbergia : subg. Muhlenbergia, with species that have phosphoenolpyruvate carboxykinase-like leaf anatomy and long, scaly rhizomes; subg. Trichochloa with long-lived species that are relatively tall (up to 3 m); subg. Clomena with 3-nerved upper glumes; sect. Pseudosporobolus species with narrow panicles and plumbeous spikelets; and sect. Bealia species with lemmas with hairy margins and midveins. Conclusions: We propose expanding the circumscription of Muhlenbergia to include the other nine genera in this subtribe and make the following new combinations: Muhlenbergia subg. Bealia, M. diandra, M. geminiflora, M. paniculata, M. phleoides, M. subg. Pseudosporobolus (also lectotipified), M. solisii, M. tricholepis. We also propose several new names: M. ammophila, M. columbi, M. plumosa. Our phylograms suggest that Muhlenbergia originated in North America because the sister (Sohnsia filifolia and Scleropogoninae) is composed of predominantly North American species. C1 [Peterson, Paul M.; Romaschenko, Konstantin] Smithsonian Inst, Dept Bot MRC 166, Natl Museum Nat Hist, Washington, DC 20013 USA. [Romaschenko, Konstantin] Bot Inst Barcelona CSIC ICUB, Lab Mol Systemat, Barcelona 08038, Spain. [Johnson, Gabriel] Smithsonian Inst, Dept Bot, Suitland, MD 20746 USA. [Johnson, Gabriel] Smithsonian Inst, Labs Analyt Biol, Suitland, MD 20746 USA. RP Peterson, PM (reprint author), Smithsonian Inst, Dept Bot MRC 166, Natl Museum Nat Hist, Washington, DC 20013 USA. EM peterson@si.edu RI Romaschenko, Konstantin/K-3096-2014 OI Romaschenko, Konstantin/0000-0002-7248-4193 FU Smithsonian Institution; National Museum of Natural History; Scholarly Studies Program; Research Opportunities, Atherton Seidell Foundation; Biodiversity Surveys and Inventories Program FX The authors thank the National Geographic Society Committee for Research and Exploration, grant number 8087-06 for field support, the Smithsonian Institution's Restricted Endowments Fund, National Museum of Natural History Small Grants Fund, the Scholarly Studies Program, Research Opportunities, Atherton Seidell Foundation, and Biodiversity Surveys and Inventories Program for financial support, J. H. Kirkbride, Jr. for translating German, A. Touwaide for correcting the Latin, and two anonymous reviewers for suggesting improvements. NR 93 TC 21 Z9 23 U1 0 U2 7 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 0002-9122 J9 AM J BOT JI Am. J. Bot. PD SEP PY 2010 VL 97 IS 9 BP 1532 EP 1554 DI 10.3732/ajb.0900359 PG 23 WC Plant Sciences SC Plant Sciences GA 646KN UT WOS:000281539000012 PM 21616906 ER PT J AU Williams, EM Gordon, AD Richmond, BG AF Williams, E. M. Gordon, A. D. Richmond, B. G. TI Upper Limb Kinematics and the Role of the Wrist During Stone Tool Production SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Article DE extension; flexion; kinematics; mechanical work; stone tool production ID KNUCKLE-WALKING ANCESTOR; HUMAN-EVOLUTION; OVERARM THROWS; EARLY HOMINID; FOSSIL EVIDENCE; MOMENT ARMS; HUMAN HAND; JOINT; TECHNOLOGY; PATTERNS AB ated the shoulder joint from the elbow and wrist joints, suggesting a shared strategy employed in other contexts (e.g., throwing) to increase target accuracy. The knapping strategy included moving the wrist into peak extension (subject peak grand mean = 47.30 degrees) at the beginning of the downswing phase, which facilitated rapid wrist flexion and accelerated the hammerstone toward the nodule. This sequence resulted in the production of significantly more mechanical work, and therefore greater strike forces, than would otherwise be produced. Together these results represent a strategy for increasing knapping efficiency in Homo sapiens and point to aspects of skeletal anatomy that might be examined to assess potential knapping ability and efficiency in fossil hominin taxa. Am J Phys Anthropol 143:134-145, 2010. (C) 2010 Wiley-Liss, Inc.Past studies have hypothesized that aspects of hominin upper limb morphology are linked to the ability to produce stone tools. However, we lack the data on upper limb motions needed to evaluate the biomechanical context of stone tool production. This study seeks to better understand the biomechanics of stone tool-making by investigating upper limb joint kinematics, focusing on the role of the wrist joint, during simple flake production. We test the hypotheses, based on studies of other upper limb activities (e.g., throwing), that upper limb movements will occur in a proximal-to-distal sequence, culminating in rapid wrist flexion just prior to strike. Data were captured from four amateur knappers during simple flake production using a VICON motion analysis system (50 Hz). Results show that subjects utilized a proximal-to-distal joint sequence and disassoci C1 [Williams, E. M.] George Washington Univ, Hominid Paleobiol Doctoral Program, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Gordon, A. D.] SUNY Albany, Dept Anthropol, Albany, NY 12222 USA. [Richmond, B. G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. RP Williams, EM (reprint author), George Washington Univ, Hominid Paleobiol Doctoral Program, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, 2110 G St NW, Washington, DC 20052 USA. EM emswill@gwmail.gwu.edu OI Gordon, Adam/0000-0002-1807-4644 FU National Science Foundation [IGERT DGE 9987590, DGE 0801634]; George Washington University; The George Washington University's Sigma Xi chapter FX Grant sponsor: National Science Foundation's Integrative Graduate Education and Research Traineeship; Grant numbers: IGERT DGE 9987590; Grant numbers: DGE 0801634. Grant sponsor: The George Washington University's Research Enhancement Fund. Grant sponsor: The George Washington University's Sigma Xi chapter. NR 69 TC 16 Z9 16 U1 4 U2 23 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 EI 1096-8644 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD SEP PY 2010 VL 143 IS 1 BP 134 EP 145 DI 10.1002/ajpa.21302 PG 12 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 643PE UT WOS:000281309500013 PM 20734439 ER PT J AU Wang, QA Smith, AL Strait, DS Wright, BW Richmond, BG Grosse, IR Byron, CD Zapata, U AF Wang, Qian Smith, Amanda L. Strait, David S. Wright, Barth W. Richmond, Brian G. Grosse, Ian R. Byron, Craig D. Zapata, Uriel TI The Global Impact of Sutures Assessed in a Finite Element Model of a Macaque Cranium SO ANATOMICAL RECORD-ADVANCES IN INTEGRATIVE ANATOMY AND EVOLUTIONARY BIOLOGY LA English DT Article DE elastic properties; structural stiffness; static loading; suture fusion; bone biomechanics ID RHESUS-MONKEY SKULLS; ELASTIC PROPERTIES; HUMAN-EVOLUTION; BONE STRAIN; CRANIOFACIAL SKELETON; MECHANICAL-PROPERTIES; COMPUTER-SIMULATION; SAGITTAL SUTURE; FACIAL SUTURES; ZYGOMATIC ARCH AB The biomechanical significance of cranial sutures in primates is an open question because their global impact is unclear, and their material properties are difficult to measure. In this study, eight suture-bone functional units representing eight facial sutures were created in a finite element model of a monkey cranium. All the sutures were assumed to have identical isotropic linear elastic material behavior that varied in different modeling experiments, representing either fused or unfused sutures. The values of elastic moduli employed in these trials ranged over several orders of magnitude. Each model was evaluated under incisor, premolar, and molar biting conditions. Results demonstrate that skulls with unfused sutures permitted more deformations and experienced higher total strain energy. However, strain patterns remained relatively unaffected away from the suture sites, and bite reaction force was likewise barely affected. These findings suggest that suture elasticity does not substantially alter load paths through the macaque skull or its underlying rigid body kinematics. An implication is that, for the purposes of finite element analysis, omitting or fusing sutures is a reasonable modeling approximation for skulls with small suture volume fraction if the research objective is to observe general patterns of craniofacial biomechanics under static loading conditions. The manner in which suture morphology and ossification affect the mechanical integrity of skulls and their ontogeny and evolution awaits further investigation,and their viscoelastic properties call for dynamic simulations. Anat Rec, 293:1477-1491, 2010. (C) 2010 Wiley-Liss, Inc. C1 [Wang, Qian; Zapata, Uriel] Mercer Univ, Sch Med, Div Basic Med Sci, Macon, GA 31207 USA. [Smith, Amanda L.; Strait, David S.] SUNY Albany, Dept Anthropol, Albany, NY 12222 USA. [Wright, Barth W.] Kansas City Univ Med & Biosci, Dept Anat, Kansas City, MO USA. [Richmond, Brian G.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC USA. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. [Grosse, Ian R.] Univ Massachusetts, Dept Mech & Ind Engn, Amherst, MA 01003 USA. [Byron, Craig D.] Mercer Univ, Dept Biol, Macon, GA 31207 USA. [Zapata, Uriel] EAFIT Univ, Dept Mech Engn, Medellin, Colombia. RP Wang, QA (reprint author), Mercer Univ, Sch Med, Div Basic Med Sci, 1550 Coll St, Macon, GA 31207 USA. EM wang_q2@mercer.edu RI Zapata M, Uriel/G-5411-2011 OI Zapata M, Uriel/0000-0002-9309-7571 FU National Science Foundation HOMINID [0725183, 0725126, 0725136, 0725078, 0725122] FX Grant sponsor: National Science Foundation HOMINID; Grant numbers: 0725183, 0725126, 0725136, 0725078, 0725122. NR 83 TC 32 Z9 34 U1 4 U2 10 PU WILEY-LISS PI HOBOKEN PA DIV JOHN WILEY & SONS INC, 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 1932-8486 J9 ANAT REC JI Anat. Rec. PD SEP PY 2010 VL 293 IS 9 BP 1477 EP 1491 DI 10.1002/ar.21203 PG 15 WC Anatomy & Morphology SC Anatomy & Morphology GA 645XC UT WOS:000281498500003 PM 20652940 ER PT J AU Crofoot, MC Lambert, TD Kays, R Wikelski, MC AF Crofoot, Margaret C. Lambert, Thomas D. Kays, Roland Wikelski, Martin C. TI Does watching a monkey change its behaviour? Quantifying observer effects in habituated wild primates using automated radiotelemetry SO ANIMAL BEHAVIOUR LA English DT Article DE Barro Colorado Island, Panama; Cebus capucinus; habituation; telemetry ID CAPUCHINS CEBUS-CAPUCINUS; FEMALE SOCIAL RELATIONSHIPS; LONG-TERM; FOREST; CHIMPANZEES; PREDATION; RESPONSES; PENGUINS; LOCATION; SURVIVAL AB In studies of animal behaviour, researchers have long been concerned that their presence may change the conduct of their study subjects. To minimize observer effects, researchers often habituate their study animals. The premise of this method is that, with sufficient neutral exposure, animals will stop reacting to humans. While numerous studies demonstrate that negative responses to humans decrease over time, the fact that an animal does not flee from or behave aggressively towards observers cannot be taken as evidence that it is not altering its behaviour in other, more subtle ways. Because remotely monitoring the behaviour of wild animals is difficult, it has not been possible to answer the critical question: do habituated animals change their behaviour when researchers are present? Here, we use data from an automated radiotelemetry system that remotely monitored the movement and activity of radiocollared animals to test whether observers affected the behaviour of seven habituated white-faced capuchins, Cebus capucinus. We found no evidence that observers influenced the ranging behaviour or activity patterns of their study subjects. Capuchins did not move faster, stop to rest less frequently, or display higher levels of activity when they were being followed compared to when they were alone. It has been suggested that researchers may embolden habituated study subjects, artificially increasing their relative dominance, but we found no relationship between observer presence and proximity to neighbouring social groups. Although it remains possible that observer effects existed but were too subtle to be detected with the remote sensing technology we used, the results of this study nevertheless provide reassuring evidence that humans can observe habituated wild animals without overly influencing the animals' activity and movement patterns. (C) 2010 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Crofoot, Margaret C.; Wikelski, Martin C.] Max Planck Inst Ornithol, Div Migrat & Immunoecol, Radolfzell am Bodensee, Germany. [Crofoot, Margaret C.; Kays, Roland; Wikelski, Martin C.] Smithsonian Trop Res Inst, Ancon, Panama. [Crofoot, Margaret C.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ USA. [Lambert, Thomas D.] Frostburg State Univ, Dept Biol, Frostburg, MD 21532 USA. [Kays, Roland] New York State Museum & Sci Serv, Albany, NY USA. RP Crofoot, MC (reprint author), Smithsonian Trop Res Inst, Unit 9100, Box 0948, Dpo, AA 34002 USA. EM crofootm@si.edu FU Frederik Sheldon Travel Grant; American Society of Primatologists; Smithsonian Tropical Research Institute; Sigma Xi; Department of Biology at Armstrong Atlantic State University; Program in Biological Anthropology, Harvard University FX We thank the Autoridad Nacional del Ambiente (ANAM) and the government of Panama for permission to conduct research in Panama, and the Smithsonian Tropical Research Institute, and especially Oris Acevedo for logistical support. Technical support was provided by the Automated Radio Telemetry System Initiative, particularly Daniel Obando, Pablo Flores, Alejandro Ortega and Kevin Sallee. We also thank Vilma Fernandez for her help collecting data, Michelle Brown, Robyn Hoing, Jennifer Boothby, Robert Horan, Vilma Fernandez and George Middleton for help with darting, Nicanor Obaldia, DVM, Claudia Brandariz, DVM and Terry Norton, DVM for veterinary support and Ben Hirsch, Scott Mangan, Ian Gilby, Susy Cote, Michelle Brown and two anonymous referees for their comments on this paper. Financial support for this work was provided by the Frederik Sheldon Travel Grant, the American Society of Primatologists, the Smithsonian Tropical Research Institute, Sigma Xi, the Department of Biology at Armstrong Atlantic State University, and the Program in Biological Anthropology, Harvard University. Required permits for the work described in this paper were obtained from the Autoridad Nacional del Ambiente, Panama, and the Smithsonian Tropical Research Institute. All research complied with the laws of the Republic of Panama and the United States of America. NR 46 TC 17 Z9 18 U1 2 U2 41 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD SEP PY 2010 VL 80 IS 3 BP 475 EP 480 DI 10.1016/j.anbehav.2010.06.006 PG 6 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 637VM UT WOS:000280846800017 ER PT J AU Winkler, U Zotz, G AF Winkler, Uwe Zotz, Gerhard TI 'And then there were three': highly efficient uptake of potassium by foliar trichomes of epiphytic bromeliads SO ANNALS OF BOTANY LA English DT Article DE Epiphytic bromeliads; potassium uptake; luxury consumption; plant nutrition; Vriesea splenriet ID MONTANE FOREST; SPANISH MOSS; PHOSPHORUS; NITROGEN; PLANTS; TRANSPORT; NUTRITION; ROOTS AB Background and ilium Vascular epiphytes have to acquire nutrients from atmospheric wash out, stem-flow, canopy soils and trapped litter. Physiological studies on the adaptations to nutrient acquisition and plant utilization of nutrients have focused on phosphorus and nitrogen; potassium, as a third highly abundant nutrient element, has received minor attention. In the present study, potassium uptake kinetics by leaves, within-plant distribution and nutrient accumulation were analysed to gain an improved understanding of physiological adaptations to non-terrestrial nutrient supply of plants. Methods Radioactively labelled (86)RbCl was used as an analogue to study uptake kinetics of potassium absorbed from tanks of epiphytes, its plant distribution and the correlation between uptake efficiency and abundance of trichomes, functioning as uptake organs of leaves. Potassium in leaves was additionally analysed by atomic absorption spectroscopy to assess plant responses to potassium deficiency. Key Results Labelled rubidium was taken up from tanks over a wide range of concentrations, 0-01-90 mM, which was achieved by two uptake systems. In four tank epiphytes, the high-affinity transporters had average K(m) values of 41-2 mu m, and the low-affinity transporters average K(m) values of 44-8 mM. Further analysis in Vriesea splenriet showed that high-affinity uptake of rubidium was an ATP-dependent process, while low-affinity uptake was mediated by a K(+)-channel. The kinetic properties of both types of transporters are comparable with those of potassium transporters in roots of terrestrial plants. Specific differences in uptake velocities of epiphytes are correlated with the abundance of trichomes on their leaf surfaces. The main sinks for potassium were fully grown leaves. These leaves thus function as internal potassium sources, which allow growth to be maintained during periods of low external potassium availability. Conclusions Vascular epiphytes possess effective mechanisms to take up potassium from both highly diluted and highly concentrated solutions, enabling the plant to incorporate this nutrient element quickly and almost quantitatively from tank solutions. A surplus not needed for current metabolism is stored, i.e. plants show luxury consumption. C1 [Winkler, Uwe; Zotz, Gerhard] Carl von Ossietzky Univ Oldenburg, Funct Ecol Grp, D-26111 Oldenburg, Germany. [Zotz, Gerhard] Smithsonian Trop Res Inst, Balboa, Panama. RP Winkler, U (reprint author), Carl von Ossietzky Univ Oldenburg, Funct Ecol Grp, D-26111 Oldenburg, Germany. EM u.winkler@uni-oldenburg.de NR 35 TC 8 Z9 8 U1 2 U2 32 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0305-7364 J9 ANN BOT-LONDON JI Ann. Bot. PD SEP PY 2010 VL 106 IS 3 BP 421 EP 427 DI 10.1093/aob/mcq120 PG 7 WC Plant Sciences SC Plant Sciences GA 648ZJ UT WOS:000281733900005 PM 20542886 ER PT J AU Uchoa, MA Nicacio, J AF Uchoa, Manoel A. Nicacio, Jose TI New Records of Neotropical Fruit Flies (Tephritidae), Lance Flies (Lonchaeidae) (Diptera: Tephritoidea), and Their Host Plants in the South Pantanal and Adjacent Areas, Brazil SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA LA English DT Article DE Anastrepha spp; Ceratitis cantata; host fruit; Neosilba spp.; taxonomy ID NEOSILBA DIPTERA; STATE; REVISION; MCALPINE AB Fruit flies (Tephritidae) and lance flies (Lonchaeidae) (Diptera) include pests of highest economic importance to horticulture around the world, because various species damage high value fruit crops. These Tephritoidea are the reason for quarantine barriers among many countries, limiting the commerce of fresh fruits and vegetables Knowledge of frugivorous tephritoid species richness and their interactions with the host plants are extremely important to Integrated Pest Management This paper presents the interactions of 15 species of Anastrepha Schiner, Ceratitis capitata (Wiedemann) (Tephritidae), and eight species of Neosilba McAlpine (Lonchaeidae) with 40 host fruit species We discovered that Pouteria glomerata (Miguel) Radlkofer (Sapotaceae) is the host fruit of Anastrepha undosa Stone. A. zernyi Ulna was associated with fruit of Anacardium othonianum Rizzini (Anacardiaceae) This is the first record of A. zernyi from the State of Mato Grosso do Sul, and of A hastata Stone from Central Brazil A sorocula Zucchi and A. zenildae Zucchi were the tephritids that infested the highest number of host fruits A alveatoides Blanchard, A. distincta Greene, A macrura Hendel, A. rheediae Stone and A. undosa Stone were recovered from only one species of host, and all of these associations are new records. Also established for the first time are the associations among eight species of Neosilba with 38 host species. N. zadolicha McAlpine and Steyskal, N. pendula (Bezzi), N glaberrima (Wiedemann) and N. mesperata Strikis and Prado were the most polyphagous Lonchaeidae C1 [Uchoa, Manoel A.; Nicacio, Jose] UFGD, Lab Insetos Frugivoros, FCBA, BR-79804970 Dourados, MS, Brazil. [Uchoa, Manoel A.] Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, Washington, DC 20013 USA. RP Uchoa, MA (reprint author), UFGD, Lab Insetos Frugivoros, FCBA, Caixa Postal 241, BR-79804970 Dourados, MS, Brazil. FU Fundacao de Apoio ao Desenvolvimento do Ensino. Ciencia e Tecnologia do Estado de Mato Grosso do Sul (FUNDECT, MS, Brazil); Conselho Nacional de Desenvolvimento Cientifico c Tecnologico (CNPq); Coodenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES) FX We thank the botanists Ubirazailda Maria Rezende from the Herbarium of the Universidade Federal de Mato Grosso do Sul (UFMS), Campo Grande-MS and Jose Rubens Pirani from the Herbarium of the Universidade de Sao Paulo (USP) Sao Paulo, Brazil, for the identification of the plant species, Pedro Carlos Strikis (UNICAMP, Campinas-SP, Brazil) for identification and mounting the Lonchaeodae, Fundacao de Apoio ao Desenvolvimento do Ensino. Ciencia e Tecnologia do Estado de Mato Grosso do Sul (FUNDECT, MS, Brazil) for the financial support to the project 'Biodiversidade de insetos frugivoros, seus hospedeiros and e immigos naturais no Brasil Central" and Conselho Nacional de Desenvolvimento Cientifico c Tecnologico (CNPq) for the grant to J N N, Coodenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES) for the Postdoctoral fellowship to M A U, and Allen L Norrboin (Systematic Entomology Laboratory, USDA-ARS) for his valuable suggestions on the manuscript, making it more comprehensive NR 46 TC 16 Z9 17 U1 0 U2 4 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0013-8746 EI 1938-2901 J9 ANN ENTOMOL SOC AM JI Ann. Entomol. Soc. Am. PD SEP PY 2010 VL 103 IS 5 BP 723 EP 733 PG 11 WC Entomology SC Entomology GA 647XY UT WOS:000281655300005 ER PT J AU Grant, JA Westall, F Beaty, DW Vago, JL AF Grant, John A. Westall, Frances Beaty, David W. Vago, Jorge L. TI Two Rovers to the Same Site on Mars, 2018: Possibilities for Cooperative Science SO ASTROBIOLOGY LA English DT Article ID SAMPLE RETURN; MISSION; EXPLORATION; SURFACE; LIFE C1 [Grant, John A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, MRC 315, Washington, DC 20013 USA. [Westall, Frances] CNRS, Ctr Biophys Mol, F-45071 Orleans 2, France. [Beaty, David W.] CALTECH, Mars Program Off, Jet Prop Lab, Pasadena, CA 91109 USA. [Vago, Jorge L.] European Space Agcy, ESA ESTEC HME ME, NL-2201 AZ Noordwijk, Netherlands. RP Grant, JA (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, MRC 315, POB 37012, Washington, DC 20013 USA. EM grantj@si.edu; frances.westall@cnrs-orleans.fr; David.Beaty@jpl.nasa.gov; Jorge.Vago@esa.int FU National Aeronautics and Space Administration FX An early draft of the list of possible options for collaborative science and their priorities (Table 2 of this report) was discussed with multiple colleagues within the Mars exploration community, including the leaders of MRR-SAG; ExoMars project leadership; the ExoMars Science Working Group; ExoMars instrument science colleagues; the JPL Mars Program Office science team; similar to 8-10 MER scientists; and professional colleagues of several team members. This resulted in the addition of several new ideas, valuable clarification of others, and refinement of our perception of their relative priorities. Chad Edwards (Chief Telecommunications Engineer, Mars Program Office, JPL) provided extensive input to the telecommunications analysis. Gerhard Kminek (Planetary Protection Officer, ESA) provided input to the section on planetary protection. An early draft of this report was presented orally on March 17, 2010, at the MEPAG meeting in Monrovia, and the ensuing discussion was very helpful in refining the ideas contained in this report. A portion of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 40 TC 4 Z9 4 U1 0 U2 7 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD SEP PY 2010 VL 10 IS 7 BP 663 EP 685 DI 10.1089/ast.2010.0526 PG 23 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 671EM UT WOS:000283483100001 ER PT J AU Laine, S Appleton, PN Gottesman, ST Ashby, MLN Garland, CA AF Laine, Seppo Appleton, Philip N. Gottesman, Stephen T. Ashby, Matthew L. N. Garland, Catherine A. TI WARM MOLECULAR HYDROGEN EMISSION IN NORMAL EDGE-ON GALAXIES NGC 4565 AND NGC 5907 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: individual (NGC 4565, NGC 5907); galaxies: ISM; galaxies: structure ID SPITZER-SPACE-TELESCOPE; INFRARED SPECTROGRAPH IRS; SPIRAL GALAXIES; ROTATION CURVES; STEPHANS QUINTET; NEUTRAL HYDROGEN; CO OBSERVATIONS; DARK-MATTER; SWS SURVEY; DUST AB We have observed warm molecular hydrogen in two nearby edge-on disk galaxies, NGC 4565 and NGC 5907, using the Spitzer high-resolution infrared spectrograph. The 0-0 S(0) 28.2 mu m and 0-0 S(1) 17.0 mu m pure rotational lines were detected out to 10 kpc from the center of each galaxy on both sides of the major axis, and in NGC 4565 the S(0) line was detected at r = 15 kpc on one side. This location is beyond the transition zone where diffuse neutral atomic hydrogen starts to dominate over cold molecular gas and marks a transition from a disk dominated by high surface-brightness far-infrared (far-IR) emission to that of a more quiescent disk. It also lies beyond a steep drop in the radio continuum emission from cosmic rays (CRs) in the disk. Despite indications that star formation activity decreases with radius, the H(2) excitation temperature and the ratio of the H(2) line and the far-IR luminosity surface densities, Sigma(L(H2))/Sigma(L(TIR)), change very little as a function of radius, even into the diffuse outer region of the disk of NGC 4565. This suggests that the source of excitation of the H(2) operates over a large range of radii and is broadly independent of the strength and relative location of UV emission from young stars. Although excitation in photodissociation regions is the most common explanation for the widespread H(2) emission, CR heating or shocks cannot be ruled out. At r = 15 kpc in NGC 4565, outside the main UV-and radio-continuum-dominated disk, we derived a higher than normal H(2) to 7.7 mu m polycyclic aromatic hydrocarbon (PAH) emission ratio, but this is likely due to a transition from mainly ionized PAH molecules in the inner disk to mainly neutral PAH molecules in the outer disk. The inferred mass surface densities of warm molecular hydrogen in both edge-on galaxies differ substantially, being 4(-60) M(circle dot)pc(-2) and 3(-50) M(circle dot)pc(-2) at r = 10 kpc for NGC 4565 and NGC 5907, respectively. The higher values represent very unlikely point-source upper limits. The point-source case is not supported by the observed emission distribution in the spectral slits. These mass surface densities cannot support the observed rotation velocities in excess of 200 km s(-1). Therefore, warm molecular hydrogen cannot account for dark matter in these disk galaxies, contrary to what was implied by a previous Infrared Space Observatory study of the nearby edge-on galaxy NGC 891. C1 [Laine, Seppo] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Appleton, Philip N.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. [Gottesman, Stephen T.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Ashby, Matthew L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Garland, Catherine A.] Castleton State Coll, Dept Nat Sci, Castleton, VT 05735 USA. RP Laine, S (reprint author), CALTECH, Spitzer Sci Ctr, MS 220-6, Pasadena, CA 91125 USA. EM seppo@ipac.caltech.edu; apple@ipac.caltech.edu; gott@astro.ufl.edu; mashby@cfa.harvard.edu; catherine.garland@castleton.edu OI Appleton, Philip/0000-0002-7607-8766 FU NASA FX We are grateful to Tom Jarrett at IPAC for helping us to correct the rogue pixels with his custom-made IRAF script. We thank the anonymous referee for very helpful and detailed comments. We acknowledge stimulating discussions with Eric Murphy on the mid-IR and far-IR properties of nearby galaxies. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. SMART was developed by the IRS Team at Cornell University and is available through the Spitzer Science Center at Caltech. The IRS was a collaborative venture between Cornell University and Ball Aerospace Corporation funded by NASA through the Jet Propulsion Laboratory and Ames Research Center. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 48 TC 8 Z9 8 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 2010 VL 140 IS 3 BP 753 EP 769 DI 10.1088/0004-6256/140/3/753 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 638GT UT WOS:000280882300009 ER PT J AU Trilling, DE Mueller, M Hora, JL Harris, AW Bhattacharya, B Bottke, WF Chesley, S Delbo, M Emery, JP Fazio, G Mainzer, A Penprase, B Smith, HA Spahr, TB Stansberry, JA Thomas, CA AF Trilling, D. E. Mueller, M. Hora, J. L. Harris, A. W. Bhattacharya, B. Bottke, W. F. Chesley, S. Delbo, M. Emery, J. P. Fazio, G. Mainzer, A. Penprase, B. Smith, H. A. Spahr, T. B. Stansberry, J. A. Thomas, C. A. TI EXPLORENEOs. I. DESCRIPTION AND FIRST RESULTS FROM THE WARM SPITZER NEAR-EARTH OBJECT SURVEY SO ASTRONOMICAL JOURNAL LA English DT Article DE minor planets, asteroids: general; infrared: planetary systems; surveys ID THERMAL INFRARED SPECTROPHOTOMETRY; KUIPER-BELT OBJECTS; SPACE-TELESCOPE; ASTEROID BELT; ARRAY CAMERA; RA-SHALOM; ORIGIN; POPULATION; MAGNITUDES; YARKOVSKY AB We have begun the ExploreNEOs project in which we observe some 700 Near-Earth Objects (NEOs) at 3.6 and 4.5 mu m with the Spitzer Space Telescope in its Warm Spitzer mode. From these measurements and catalog optical photometry we derive albedos and diameters of the observed targets. The overall goal of our ExploreNEOs program is to study the history of near-Earth space by deriving the physical properties of a large number of NEOs. In this paper, we describe both the scientific and technical construction of our ExploreNEOs program. We present our observational, photometric, and thermal modeling techniques. We present results from the first 101 targets observed in this program. We find that the distribution of albedos in this first sample is quite broad, probably indicating a wide range of compositions within the NEO population. Many objects smaller than 1 km have high albedos (greater than or similar to 0.35), but few objects larger than 1 km have high albedos. This result is consistent with the idea that these larger objects are collisionally older, and therefore possess surfaces that are more space weathered and therefore darker, or are not subject to other surface rejuvenating events as frequently as smaller NEOs. C1 [Trilling, D. E.; Thomas, C. A.] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86001 USA. [Mueller, M.; Delbo, M.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice 4, France. [Hora, J. L.; Fazio, G.; Smith, H. A.; Spahr, T. B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Harris, A. W.] DLR Inst Planetary Res, D-12489 Berlin, Germany. [Bhattacharya, B.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. [Bottke, W. F.] SW Res Inst, Boulder, CO 80302 USA. [Chesley, S.; Mainzer, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Emery, J. P.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Penprase, B.] Pomona Coll, Dept Phys & Astron, Claremont, CA 91711 USA. [Stansberry, J. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Trilling, DE (reprint author), No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86001 USA. EM david.trilling@nau.edu OI Mueller, Michael/0000-0003-3217-5385; Hora, Joseph/0000-0002-5599-4650; Thomas, Cristina/0000-0003-3091-5757 FU NASA FX We acknowledge the thorough and prompt hard work of the staff at the Spitzer Science Center, without whom the execution of this program would not be possible. We thank Michael Mommert (DLR) for help in checking the modeling results given in the data tables. We thank an anonymous referee for making a number of useful suggestions. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by JPL/Caltech under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 68 TC 29 Z9 29 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 2010 VL 140 IS 3 BP 770 EP 784 DI 10.1088/0004-6256/140/3/770 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 638GT UT WOS:000280882300010 ER PT J AU Song, LM Tripp, TM Wang, QD Yao, YS Cui, W Xue, YQ Orosz, JA Steeghs, D Steiner, JF Torres, MAP McClintock, JE AF Song, Limin Tripp, Todd M. Wang, Q. Daniel Yao, Yangsen Cui, Wei Xue, Yongquan Orosz, Jerome A. Steeghs, Danny Steiner, James F. Torres, Manuel A. P. McClintock, Jeffrey E. TI VARIABLE O vi AND N v EMISSION FROM THE X-RAY BINARY LMC X-3: HEATING OF THE BLACK HOLE COMPANION SO ASTRONOMICAL JOURNAL LA English DT Article DE stars: individual (LMCX-3) ID ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; INTERSTELLAR-MEDIUM; ACCRETION DISK; STELLAR WINDS; SPECTROGRAPH; LMC-X-3; STARS; MODEL; HALO; OVI AB Based on high-resolution ultraviolet spectroscopy obtained with the Far Ultraviolet Spectroscopic Explorer (FUSE) and the Cosmic Origins Spectrograph, we present new detections of Ovi and Nv emission from the black hole X-ray binary (XRB) system LMCX-3. We also update the ephemeris of the XRB using recent radial velocity measurements obtained with the echelle spectrograph on the Magellan-Clay telescope. We observe significant velocity variability of the UV emission, and we find that the Ovi and Nv emission velocities follow the optical velocity curve of the XRB. Moreover, the Ovi and Nv intensities regularly decrease between binary phase=0.5 and 1.0, which suggests that the source of the UV emission is increasingly occulted as the B star in the XRB moves from superior to inferior conjunction. These trends suggest that illumination of the B star atmosphere by the intense X-ray emission from the accreting black hole creates a hot spot on one side of the B star, and this hot spot is the origin of the Ovi and Nv emission. However, the velocity semiamplitude of the ultraviolet emission, K(UV) approximate to 180 km s(-1), is lower than the optical semiamplitude; this difference could be due to rotation of the B star. Comparison of the FUSE observations taken in 2001 November and 2004 April shows a significant change in the Ovi emission characteristics: in the 2001 data, the Ovi region shows both broad and narrow emission features, while in 2004 only the narrow Ovi emission is clearly present. Rossi X-ray Timing Explorer data show that the XRB was in a high/soft state in the 2001 November epoch but was in a transitional state in 2004 April, so the shape of the X-ray spectrum might change the properties of the region illuminated on the B star and thus change the broad versus narrow characteristics of the UV emission. If our hypothesis about the origin of the highly ionized emission is correct, then careful analysis of the emission occultation could, in principle, constrain the inclination of the XRB and the mass of the black hole. Key words: stars: individual (LMCX-3) C1 [Song, Limin; Tripp, Todd M.; Wang, Q. Daniel] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Yao, Yangsen] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Cui, Wei; Xue, Yongquan] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Xue, Yongquan] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Steeghs, Danny] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Steiner, James F.; Torres, Manuel A. P.; McClintock, Jeffrey E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Song, LM (reprint author), Univ Massachusetts, Dept Astron, Lederle Grad Res Tower B 619E,710 N Pleasant St, Amherst, MA 01003 USA. RI Steeghs, Danny/C-5468-2009; OI Steeghs, Danny/0000-0003-0771-4746; Cui, Wei/0000-0002-6324-5772 FU NASA [NNG04GJB83G, HST-GO-11642.01-A, HST-GO-11642.02-A] FX We thank John Raymond, Saku Vrtilek, and Jifeng Liu for their very helpful comments on an early version of the paper. We thank the referee for thoughtful suggestions. The data presented in this paper were obtained for the FUSE GO program E063 and the HST GO program 11642. These programs were funded by NASA through grants NNG04GJB83G, HST-GO-11642.01-A, and HST-GO-11642.02-A, respectively. NR 26 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 2010 VL 140 IS 3 BP 794 EP 803 DI 10.1088/0004-6256/140/3/794 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 638GT UT WOS:000280882300012 ER PT J AU Hughes, AM Andrews, SM Wilner, DJ Meyer, MR Carpenter, JM Qi, C Hales, AS Casassus, S Hogerheijde, MR Mamajek, EE Wolf, S Henning, T Silverstone, MD AF Hughes, A. M. Andrews, S. M. Wilner, D. J. Meyer, M. R. Carpenter, J. M. Qi, C. Hales, A. S. Casassus, S. Hogerheijde, M. R. Mamajek, E. E. Wolf, S. Henning, T. Silverstone, M. D. TI STRUCTURE AND COMPOSITION OF TWO TRANSITIONAL CIRCUMSTELLAR DISKS IN CORONA AUSTRALIS SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; protoplanetary disks; stars: individual (RX J1842.9-3532, RX J1852.3-3700); stars: pre-main sequence ID T-TAURI STARS; 2-DIMENSIONAL RADIATIVE-TRANSFER; MAIN-SEQUENCE STARS; SUN-LIKE STARS; PROTOPLANETARY DISKS; PLANETARY SYSTEMS; YOUNG STARS; X-RAY; SUBMILLIMETER ARRAY; ACCRETION RATES AB The late stages of evolution of the primordial circumstellar disks surrounding young stars are poorly understood, yet vital to constraining theories of planet formation. We consider basic structural models for the disks around two similar to 10 Myr old members of the nearby RCrA association: RX J1842.9-3532 and RX J1852.3-3700. We present new arc second-resolution maps of their 230 GHz continuum emission from the Submillimeter Array and unresolved CO(3-2) spectra from the Atacama Submillimeter Telescope Experiment. By combining these data with broadband fluxes from the literature and infrared fluxes and spectra from the catalog of the Formation and Evolution of Planetary Systems Legacy program on the Spitzer Space Telescope, we assemble a multiwavelength data set probing the gas and dust disks. Using the Monte Carlo radiative transfer code RADMC to model simultaneously the spectral energy distribution and millimeter continuum visibilities, we derive basic dust disk properties and identify an inner cavity of radius 16 AU in the disk around RX J1852.3-3700. We also identify an optically thin 5 AU cavity in the disk around RX J1842.9-3532, with a small amount of optically thick material close to the star. The molecular line observations suggest an intermediate disk inclination in RX J1842.9-3532, consistent with the continuum emission. In combination with the dust models, the molecular data allow us to derive a lower CO content than expected, suggesting that the process of gas clearing is likely underway in both systems, perhaps simultaneously with planet formation. C1 [Hughes, A. M.; Andrews, S. M.; Wilner, D. J.; Qi, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Meyer, M. R.] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland. [Carpenter, J. M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Hales, A. S.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Casassus, S.] Univ Chile, Dept Astron, Santiago, Chile. [Hogerheijde, M. R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Mamajek, E. E.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Wolf, S.] Univ Kiel, Inst Theoret Phys & Astrophys, D-24098 Kiel, Germany. [Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Silverstone, M. D.] Eureka Sci Inc, Cary, NC 27513 USA. RP Hughes, AM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mhughes@cfa.harvard.edu; sandrews@cfa.harvard.edu; dwilner@cfa.harvard.edu; mmeyer@phys.ethz.ch; jmc@astro.caltech.edu; cqi@cfa.harvard.edu; ahales@alma.cl; simon@das.uchile.cl; michiel@strw.leidenuniv.nl; emamajek@pas.rochester.edu; wolf@astrophysik.uni-kiel.de; henning@mpia-hd.mpg.de; mdsilverstone@att.net RI Casassus, Simon/I-8609-2016 FU NASA [NAG5-11777, NAS 5-26555, NNG06GH25G]; Space Telescope Science Institute FX We thank C. P. Dullemond for access to the two-dimensional version of RADMC. Partial support for this work was provided by NASA Origins of Solar Systems Program Grant NAG5-11777. A. M. H. acknowledges support from a National Science Foundation Graduate Research Fellowship. Support for S. M. A. was provided by NASA through Hubble Fellowship grant HF-01203-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. M. R. M. acknowledges the Harvard Origins of Life Initiative, the Smithsonian Astrophysical Observatory, and a NASA TPF Foundation Science Program grant NNG06GH25G (PI: S. Kenyon) for sabbatical support. NR 66 TC 18 Z9 18 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 2010 VL 140 IS 3 BP 887 EP 896 DI 10.1088/0004-6256/140/3/887 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 638GT UT WOS:000280882300019 ER PT J AU Castelli, F Kurucz, RL AF Castelli, F. Kurucz, R. L. TI New Fe II energy levels from stellar spectra SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE line: identification; atomic data; stars: atmospheres; stars: chemically peculiar; stars: individual: HR 6000 ID SUPERMULTIPLET; LINES AB Aims. The spectra of B-type and early A-type stars show numerous unidentified lines in the whole optical range, especially in the 5100-5400 angstrom interval. Because Fe II transitions to high energy levels should be observed in this region, we used semiempirical predicted wavelengths and gf-values of Fe II to identify unknown lines. Methods. Semiempirical line data for Fe II computed by Kurucz are used to synthesize the spectrum of the slow-rotating, Fe-overabundant CP star HR 6000. Results. We determined a total of 109 new 4f levels for Fe II with energies ranging from 122 324 cm(-1) to 128 110 cm(-1). They belong to the Fe II subconfigurations 3d(6)((3)P)4f (10 levels), 3d(6)((3)H)4f (36 levels), 3d(6)((3)F)4f (37 levels), and 3d(6)((3)G)4f (26 levels). We also found 14 even levels from 4d (3 levels), 5d (7 levels), and 6d (4 levels) configurations. The new levels have allowed us to identify more than 50% of the previously unidentified lines of HR 6000 in the wavelength region 3800-8000 angstrom. Tables listing the new energy levels are given in the paper; tables listing the spectral lines with log gf >= -1.5 that are transitions to the 4f energy levels are given in the Online Material. These new levels produce 18 000 lines throughout the spectrum from the ultraviolet to the infrared. C1 [Castelli, F.] Ist Nazl Astrofis, Osservatorio Astron Trieste, I-34131 Trieste, Italy. [Kurucz, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Castelli, F (reprint author), Ist Nazl Astrofis, Osservatorio Astron Trieste, Via Tiepolo 11, I-34131 Trieste, Italy. EM castelli@oats.inaf.it NR 13 TC 16 Z9 16 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP-OCT PY 2010 VL 520 AR A57 DI 10.1051/0004-6361/201015126 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 665VQ UT WOS:000283064200117 ER PT J AU Israel, H Erben, T Reiprich, TH Vikhlinin, A Hildebrandt, H Hudson, DS McLeod, BA Sarazin, CL Schneider, P Zhang, YY AF Israel, H. Erben, T. Reiprich, T. H. Vikhlinin, A. Hildebrandt, H. Hudson, D. S. McLeod, B. A. Sarazin, C. L. Schneider, P. Zhang, Y. -Y. TI The 400d Galaxy Cluster Survey weak lensing programme I. MMT/Megacam analysis of CL0030+2618 at z=0.50 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individuals: CL0030+2618; cosmology: observations gravitational lensing: weak; X-rays: galaxies: clusters ID BONN DEEP SURVEY; COSMIC SHEAR ANALYSIS; LYMAN-BREAK GALAXIES; DARK-MATTER HALOES; DIGITAL SKY SURVEY; X-RAY SOURCES; MASS FUNCTION; PHOTOMETRIC REDSHIFTS; OBSERVED GROWTH; PUBLIC-SURVEY AB Context. Studying cosmological structure formation provides insights into all of the universe's components: baryonic matter, dark matter, and, notably, dark energy. Measuring the mass function of galaxy clusters at high redshifts is particularly useful probe for both learning about the history of structure formation and constraining cosmological parameters. Aims. We attempt to derive reliable masses for a high-redshift, high-luminosity sample of galaxy clusters selected from the 400d X-ray selected cluster survey. Weak gravitational lensing allows us to determine masses that can be compared with those inferred from X-rays, forming an independent test. We focus on a particular object, CL0030+2618 at z = 0.50. Methods. Using deep imaging in three passbands acquired using the Megacam instrument at MMT, we show that Megacam is well-suited to measuring gravitational shear, i.e., the shapes of faint galaxies. A catalogue of background galaxies is constructed by analysing the photometric properties of galaxies in the g'r'i' bands. Results. Using the aperture mass technique, we detect the weak lensing signal of CL0030+2618 at 5.8 sigma significance. We find significant tangential alignment of galaxies out to similar to 10' or a distance of >2 r(200) from the cluster centre. The weak lensing centre of CL0030+2618 agrees with several X-ray measurements and the position of the brightest cluster galaxy. Finally, we infer a weak lensing virial mass of M(200) = 7.2(-2.9-2.5)(+ 3.6+2.3) x 10(14) M(circle dot) for CL0030+2618. Conclusions. Despite complications caused by a tentative foreground galaxy group along the line of sight, the X-ray and weak lensing estimates for CL0030+2618 are in remarkable agreement. C1 [Israel, H.; Erben, T.; Reiprich, T. H.; Hudson, D. S.; Schneider, P.; Zhang, Y. -Y.] Argelander Inst Astron, D-53121 Bonn, Germany. [Vikhlinin, A.; McLeod, B. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hildebrandt, H.] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands. [Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. RP Israel, H (reprint author), Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany. EM hisrael@astro.uni-bonn.de FU Silicon Valley Community Foundation; Smithsonian Astrophysical Observatory; NOAO; NSF FX Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. Our MMT observations were supported in part by a donation from the F. H. Levinson Fund of the Silicon Valley Community Foundation to the University of Virginia. In addition, MMT observations used for this project were granted by the Smithsonian Astrophysical Observatory and by NOAO, through the Telescope System Instrumentation Program (TSIP). TSIP is funded by NSF. NR 92 TC 20 Z9 20 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP-OCT PY 2010 VL 520 AR A58 DI 10.1051/0004-6361/200913667 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 665VQ UT WOS:000283064200033 ER PT J AU Kalkofen, W Rossi, P Bodo, G Massaglia, S AF Kalkofen, W. Rossi, P. Bodo, G. Massaglia, S. TI Acoustic waves in a stratified atmosphere IV. Three-dimensional nonlinear hydrodynamics SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE hydrodynamics; stars: late-type; waves; Sun: chromosphere ID SOLAR CHROMOSPHERE; PROPAGATION; INTERNETWORK; OSCILLATIONS; EXCITATION; DYNAMICS; GRAINS; ENERGY; SUMER AB Context. The quiet solar chromosphere in the interior of supergranulation cells is believed to be heated by the dissipation of acoustic waves that originate with a typical period of 3 min in the photosphere. Aims. We investigate how the horizontal expansion with height of acoustic waves traveling upward into an isothermal, gravitationally stratified atmosphere depends on the size of the source region. Methods. We have solved the three-dimensional, nonlinear, time-dependent hydrodynamic equations for impulsively-generated, upward-propagating acoustic waves, assuming cylindrical symmetry. Results. When the diameter of the source of acoustic waves is small, the pattern of the upward-propagating waves is that of a point source, for which the energy travels upward in a vertical cone, qualitatively matching the observed pattern of bright-point expansion with height. For the largest plausible size of a source region, i.e., with granular size of 1 Mm, wave propagation in the low chromosphere is approximately that of plane waves, but in the middle and upper chromosphere it is also that of a point source. The assumption of plane-wave propagation is not a good approximation in the solar chromosphere. The upward-directed energy flux is larger than that of the solar chromosphere, at least in the middle and upper chromosphere, and probably throughout. Conclusions. Simulations of impulsively generated acoustic waves emitted from source regions with diameters that are small compared to the pressure scale height of the atmosphere qualitatively reproduce the upward expansion observed in chromospheric bright points. The emission features in the cores of the H and K lines are predicted to be blueshifted for a pulse and redshifted for the waves in its wake. The contribution of internal gravity waves to the upward energy flux is small and decreases with increasing size of the source region. C1 [Kalkofen, W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kalkofen, W.] Kiepenheuer Inst Solar Phys, D-79104 Freiburg, Germany. [Rossi, P.; Bodo, G.] INAF Osservatorio Astron Torino, I-10025 Pino Torinese, Italy. [Massaglia, S.] Univ Torino, Dipartimento Fis Gen, I-10125 Turin, Italy. RP Kalkofen, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM wkalkofen@cfa.harvard.edu; rossi@oato.inaf.it; bodo@oato.inaf.it; massaglia@ph.unito.it RI Bodo, Gianluigi/F-9223-2012; ROSSI, PAOLA/I-7031-2015 OI Bodo, Gianluigi/0000-0002-9265-4081; massaglia, silvano/0000-0003-1779-7426; ROSSI, PAOLA/0000-0002-0840-4726 NR 32 TC 6 Z9 6 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP-OCT PY 2010 VL 520 AR A100 DI 10.1051/0004-6361/200912996 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 665VQ UT WOS:000283064200100 ER PT J AU Robitaille, TP AF Robitaille, T. P. TI On the modified random walk algorithm for Monte-Carlo radiation transfer (Research Note) SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE radiative transfer; diffusion; circumstellar matter; methods: numerical AB Min et al. (2009) presented two complementary techniques that use the diffusion approximation to allow efficient Monte-Carlo radiation transfer in very optically thick regions: a modified random walk and a partial diffusion approximation. In this note, I show that the calculations required for the modified random walk method can be significantly simplified. In particular, the diffusion coefficient and the mass absorption coefficients required for the modified random walk are in fact the same as the standard diffusion coefficient and the Planck mean mass absorption coefficient. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Robitaille, TP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM trobitaille@cfa.harvard.edu OI Robitaille, Thomas/0000-0002-8642-1329 FU NASA; Jet Propulsion Laboratory, California Institute of Technology FX I wish to thank the referee for a careful review, and for insightful comments that improved this research note. I also wish to thank Barbara Whitney, Kenny Wood, and Katharine Johnston for useful discussions. Support for this work was provided by NASA through the Spitzer Space Telescope Fellowship Program, through a contract issued by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. NR 3 TC 15 Z9 15 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP-OCT PY 2010 VL 520 AR A70 DI 10.1051/0004-6361/201015025 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 665VQ UT WOS:000283064200128 ER PT J AU Strassmeier, KG Granzer, T Kopf, M Weber, M Kuker, M Reegen, P Rice, JB Matthews, JM Kuschnig, R Rowe, JF Guenther, DB Moffat, AFJ Rucinski, SM Sasselov, D Weiss, WW AF Strassmeier, K. G. Granzer, T. Kopf, M. Weber, M. Kueker, M. Reegen, P. Rice, J. B. Matthews, J. M. Kuschnig, R. Rowe, J. F. Guenther, D. B. Moffat, A. F. J. Rucinski, S. M. Sasselov, D. Weiss, W. W. TI Rotation and magnetic activity of the Hertzsprung-gap giant 31 Comae SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: activity; stars: atmospheres; stars: individual: 31 Comae; starspots; stars: late-type; stars: rotation ID PRE-MAIN-SEQUENCE; LATE-TYPE STARS; GENEVA-COPENHAGEN SURVEY; TIME-SERIES ANALYSIS; X-RAY ACTIVITY; LATE A-TYPE; G-K GIANTS; STELLAR EVOLUTION; COOL STARS; LUMINOSITY CLASSIFICATION AB Context. The single rapidly-rotating G0 giant 31 Comae has been a puzzle because of the absence of photometric variability despite its strong chromospheric and coronal emissions. As a Hertzsprung-gap giant, it is expected to be at the stage of rearranging its moment of inertia, hence likely also its dynamo action, which could possibly be linked with its missing photospheric activity. Aims. Our aim is to detect photospheric activity, obtain the rotation period, and use it for a first Doppler image of the star's surface. Its morphology could be related to the evolutionary status. Methods. We carried out high-precision, white-light photometry with the MOST satellite, ground-based Stromgren photometry with automated telescopes, and high-resolution optical echelle spectroscopy with the new STELLA robotic facility. Results. The MOST data reveal, for the first time, light variations with a full amplitude of 5 mmag and an average photometric period of 6.80 +/- 0.06 days. Radial-velocity variations with a full amplitude of 270 ms(-1) and a period of 6.76 +/- 0.02 days were detected from our STELLA spectra, which we also interpret as due to stellar rotation. The two-year constancy of the average radial velocity of +0.10 +/- 0.33 km s(-1) confirms the star's single status, as well as the membership in the cluster Melotte 111. A spectrum synthesis gives T-eff = 5660 +/- 42 K, log g = 3.51 +/- 0.09, and [Fe/H] = -0.15 +/- 0.03, which together with the revised Hipparcos distance, suggests a mass of 2.6 +/- 0.1 M-circle dot and an age of approximate to 540 Myr. The surface lithium abundance is measured to be nearly primordial. A detection of a strong He I absorption line indicates nonradiative heating processes in the atmosphere. Our Doppler images show a large, asymmetric polar spot, cooler than Teff by approximate to 1600 K, and several small low-to-mid latitude features that are warmer by approximate to 300-400 K and are possibly of chromospheric origin. We computed the convective turnover time for 31 Com as a function of depth and found on average tau(C) approximate to 5 days. Conclusions. 31 Com appears to be just at the onset of rapid magnetic braking and Li dilution because its age almost exactly coincides with the predicted onset of envelope convection. That we recover a big polar starspot despite the Rossby number being larger than unity, and thus no efficient (envelope) dynamo is expected, leads us to conclude that 31 Com still harbors a fossil predominantly poloidal magnetic field. However, the increasing convective envelope may have just started an interface dynamo that now is the source of the warm surface features and the corresponding UV and X-ray emission. C1 [Strassmeier, K. G.; Granzer, T.; Kopf, M.; Weber, M.; Kueker, M.] AIP, D-14482 Potsdam, Germany. [Reegen, P.; Kuschnig, R.; Weiss, W. W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Rice, J. B.] Brandon Univ, Dept Phys, Brandon, MB R7A 6A9, Canada. [Matthews, J. M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Rowe, J. F.] NASA Ames Res Ctr, Moffett Field, CA 94035 USA. [Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Moffat, A. F. J.] Univ Montreal CP 6128, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Rucinski, S. M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON OM5S 3H4, Canada. [Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Strassmeier, KG (reprint author), AIP, Sternwarte 16, D-14482 Potsdam, Germany. EM kstrassmeier@aip.de; reegen@astro.univie.ac.at; rice@BrandonU.ca FU Natural Sciences and Engineering Research Council (NSERC) Canada; Canadian Space Agency; Austrian Science Promotion Agency (FFG-MOST); Austrian Science Funds [FWF-P17580]; FWF; KGS FX K.G.S. and the AIP coauthors are grateful to the State of Brandenburg and the German federal ministry for education and research (BMBF) for their continuous support of the STELLA and APT activities. It is our pleasure to thank Sydney Barnes and Yong-Cheol Kim for computing the moment-of-inertia models for us. We particularly thank our anonymous referee whose comments resulted in a much improved paper. J.B.R., J.M.M., D.B.G., A.F.J.M., and S.M.R. are supported by funding from the Natural Sciences and Engineering Research Council (NSERC) Canada. R.K. is funded by the Canadian Space Agency. W.W.W. is supported by the Austrian Science Promotion Agency (FFG-MOST) and the Austrian Science Funds (FWF-P17580). The APT operation has been supported by grants from the FWF to M. Breger and KGS. This work has made use of BaSTI web tools, the MESA code and of the many CDS-Strasbourg services. NR 120 TC 10 Z9 10 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP-OCT PY 2010 VL 520 AR A52 DI 10.1051/0004-6361/201015023 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 665VQ UT WOS:000283064200075 ER PT J AU Gunther, HM Matt, SP Schmitt, JHMM Gudel, M Li, ZY Burton, DM AF Guenther, H. M. Matt, S. P. Schmitt, J. H. M. M. Guedel, M. Li, Z. -Y. Burton, D. M. TI The disk-bearing young star IM Lupi X-ray properties and limits on accretion SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; stars: individual: IM Lup; X-rays: stars ID T-TAURI-STARS; MAIN-SEQUENCE STARS; NEWTON EXTENDED SURVEY; LOW-MASS STARS; EMISSION-LINES; BROWN DWARFS; MAGNETOSPHERIC ACCRETION; MOLECULAR CLOUD; ATOMIC DATABASE; HERBIG STAR AB Context. Classical T Tauri stars (CTTS) differ in their X-ray signatures from older pre-main sequence stars, e.g., weak-lined TTS (WTTS). CTTS exhibit a soft excess and deviations from the low-density coronal limit in the He-like triplets. Aims. We test whether these features correlate with either accretion or the presence of a disk by observing IM Lup, a disk-bearing object apparently in transition between CTTS and WTTS without obvious accretion. Methods. We analyse a Chandra grating spectrum and additional XMM-Newton data of IM Lup and accompanying optical spectra, some of which where taken simultaneously with the X-ray observations. We fit the X-ray emission lines and decompose the H alpha emission line into different components. Results. In X-rays, IM Lup has a bright and hot active corona, where elements with low first-ionisation potential are depleted. The He-like Ne IX triplet is in the low-density state, but because of the small number of counts in the data a high-density scenario cannot be excluded at the 90% confidence level. In terms of all its X-ray properties, IM Lup resembles a main-sequence star, but is also compatible with CTTS signatures at the 90% confidence level, thus we cannot decide whether the soft excess and deviations from the low-density coronal limit for the He-like triplets in CTTS are produced by accretion or only the presence of a disk. The star IM Lup is chromospherically active, which accounts for most of its emission in H alpha. Despite its low equivalent width, the complexity of the H alpha line profile is reminiscent of CTTS. We estimate the mass accretion rate to be 10(-11) M(circle dot) yr(-1). C1 [Guenther, H. M.; Schmitt, J. H. M. M.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. [Guenther, H. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Matt, S. P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Guedel, M.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Guedel, M.] Univ Vienna, Dept Astron, A-1180 Vienna, Austria. [Li, Z. -Y.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Burton, D. M.] Univ So Queensland, Toowoomba, Qld 4350, Australia. RP Gunther, HM (reprint author), Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. EM moritz.guenther@hs.uni-hamburg.de RI Guedel, Manuel/C-8486-2015; OI Guedel, Manuel/0000-0001-9818-0588; Gunther, Hans Moritz/0000-0003-4243-2840; Matt, Sean/0000-0001-9590-2274 FU ESA Member States; NASA; NRL (USA); RAL (UK); MSSL (UK); Universities of Florence (Italy); Cambridge (UK); George Mason University (USA); La Silla Observatory [081.C-0779(A)]; DLR [50OR0105]; Oak Ridge Associated Universities; Chandra [GO9-0007X] FX Based on observations obtained with XMM-Newton, an ESA science mission, and Chandra, a NASA science mission, both with instruments and contributions directly funded by ESA Member States and NASA.; CHIANTI is a collaborative project involving the NRL (USA), RAL (UK), MSSL (UK), the Universities of Florence (Italy) and Cambridge (UK), and George Mason University (USA). We made use of observations made with ESO Telescopes at the La Silla Observatory under programme ID 081.C-0779(A). The authors would like to thank Ian Waite, USQ, for the initial extraction of the IM Lup data from ANU. H.M.G. acknowledges support from DLR under 50OR0105. S.P.M. was supported by an appointment to the NASA Postdoctoral Program at Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. Z.-Y.L. acknowledges support from Chandra grant GO9-0007X. NR 66 TC 5 Z9 5 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2010 VL 519 AR A97 DI 10.1051/0004-6361/201014386 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 668UQ UT WOS:000283297300097 ER PT J AU Krivonos, R Revnivtsev, M Tsygankov, S Sazonov, S Vikhlinin, A Pavlinsky, M Churazov, E Sunyaev, R AF Krivonos, R. Revnivtsev, M. Tsygankov, S. Sazonov, S. Vikhlinin, A. Pavlinsky, M. Churazov, E. Sunyaev, R. TI INTEGRAL/IBIS 7-year All-Sky Hard X-ray Survey I. Image reconstruction SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: data analysis; methods: observational; techniques: image processing; surveys; X-rays: general; Galaxy: general ID UNIFORMLY REDUNDANT ARRAYS; GALACTIC PLANE SCAN; SURVEY CATALOG; WAVELET TRANSFORM; IBIS TELESCOPE; COMA CLUSTER; REGION; EMISSION; MISSION; RIDGE AB This paper is the first in a series devoted to the hard X-ray whole sky survey performed by the INTEGRAL observatory over seven years. Here we present an improved method for image reconstruction with the IBIS coded mask telescope. The main improvements are related to the suppression of systematic effects that strongly limit sensitivity in the region of the Galactic plane (GP), especially in the crowded field of the Galactic center (GC). We extended the IBIS/ISGRI background model to take into account the Galactic ridge X-ray emission (GRXE). To suppress residual systematic artifacts on a reconstructed sky image, we applied nonparametric sky image filtering based on wavelet decomposition. The implemented modifications of the sky reconstruction method decrease the systematic noise in the similar to 20 Ms deep field of GC by similar to 44%, and practically remove it from the high-latitude sky images. New observational data sets, along with an improved reconstruction algorithm, allow us to conduct the hard X-ray survey with the best currently available minimal sensitivity 3.7 x 10(-12) erg s(-1) cm(-2) similar to 0.26 mCrab in the 17-60 keV band at a 5 sigma detection level. The survey covers 90% of the sky down to the flux limit of 6.2 x 10(-11) erg s(-1) cm(-2) (similar to 4.32 mCrab) and 10% of the sky area down to the flux limit of 8.6 x 10(-12) erg s(-1) cm(-2) (similar to 0.60 mCrab). C1 [Krivonos, R.; Tsygankov, S.; Churazov, E.; Sunyaev, R.] Max Planck Inst Astrophys, D-85740 Garching, Germany. [Krivonos, R.; Revnivtsev, M.; Tsygankov, S.; Sazonov, S.; Vikhlinin, A.; Pavlinsky, M.; Churazov, E.; Sunyaev, R.] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. [Revnivtsev, M.] Tech Univ Munich, D-85748 Garching, Germany. [Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Krivonos, R (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85740 Garching, Germany. EM krivonos@mpa-garching.mpg.de RI Churazov, Eugene/A-7783-2013 FU Russian Federation [NSH-5069.2010.2]; Presidium of the Russian Academy of Sciences/RAS; Division of Physical Sciences of the RAS [OFN-17]; Russian Basic Research Foundation [09-02-00867]; Dynasty Foundation; ESA, Denmark; ESA, France; ESA, Germany; ESA, Italy; ESA, Switzerland; ESA, Spain; ESA, Czech Republic; ESA, Poland FX We are grateful to the anonymous referee for the critical remarks that helped us improve the paper. The data used were from the European and Russian INTEGRAL Science Data Centers2,3. The work was supported by the President of the Russian Federation (through the program supporting leading scientific schools, project NSH-5069.2010.2), by the Presidium of the Russian Academy of Sciences/RAS (the program "Origin, Structure, and Evolution of Objects of the Universe"), by the Division of Physical Sciences of the RAS (the program "Extended objects in the Universe", OFN-17), and by the Russian Basic Research Foundation (project 09-02-00867). S. S. acknowledges the support of the Dynasty Foundation. R. K. would like to express his sincere gratitude to Kate O'Shea for her support in the preparation of the paper.; Based on observations with INTEGRAL, an ESA project with the instruments and science data center funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland, Spain), Czech Republic, and Poland, and with the participation of Russia and the USA. NR 42 TC 32 Z9 32 U1 1 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2010 VL 519 AR A107 DI 10.1051/0004-6361/200913814 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 668UQ UT WOS:000283297300107 ER PT J AU Lombardi, M Alves, J Lada, CJ AF Lombardi, M. Alves, J. Lada, C. J. TI Larson's third law and the universality of molecular cloud structure SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: clouds; dust, extinction; ISM: structure; methods: statistical ID FIELD EXTINCTION MAPS; DUST; COMPLEXES; MASS; GAS AB Larson (1981) first noted a scaling relation between masses and sizes in molecular clouds that implies that these objects have approximately constant column densities. This original claim, based upon millimeter observations of carbon monoxide lines, has been challenged by many theorists, arguing that the apparent constant column density observed is merely the result of the limited dynamic range of observations, and that in reality clouds have column density variations over two orders of magnitudes. In this letter we investigate a set of nearby molecular clouds with near-infrared excess methods, which guarantee very large dynamic ranges and robust column density measurements, to test the validity of Larson's third law. We verify that different clouds have almost identical average column densities above a given extinction threshold; this holds regardless of the extinction threshold, but the actual average surface mass density is a function of the specific threshold used. We show that a second version of Larson's third law, involving the mass-radius relation for single clouds and cores, does not hold in our sample, indicating that individual clouds are not objects that can be described by constant column density. Our results instead indicate that molecular clouds are characterized by a universal structure. Finally we point out that this universal structure can be linked to the log-normal nature of cloud column density distributions. C1 [Lombardi, M.] Univ Milan, Dept Phys, I-20133 Milan, Italy. [Lombardi, M.] European So Observ, D-85748 Garching, Germany. [Alves, J.] Univ Vienna, A-1180 Vienna, Austria. [Lada, C. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lombardi, M (reprint author), Univ Milan, Dept Phys, Via Celoria 16, I-20133 Milan, Italy. EM mlombard@eso.org OI LOMBARDI, MARCO/0000-0002-3336-4965; Alves, Joao/0000-0002-4355-0921 NR 26 TC 36 Z9 36 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2010 VL 519 AR L7 DI 10.1051/0004-6361/201015282 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 668UQ UT WOS:000283297300124 ER PT J AU Wagg, J Carilli, CL Wilner, DJ Cox, P De Breuck, C Menten, K Riechers, DA Walter, F AF Wagg, J. Carilli, C. L. Wilner, D. J. Cox, P. De Breuck, C. Menten, K. Riechers, D. A. Walter, F. TI [CII] line emission in BRI 1335-0417 at z=4.4 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: high-redshift; galaxies: ISM ID C-II LINE; FAR-INFRARED SPECTROSCOPY; QUASAR HOST GALAXY; HIGH-REDSHIFT; STAR-FORMATION; MOLECULAR GAS; BIG-BANG; MU-M; STARBURST; QSOS AB Using the 12-m APEX telescope, we have detected redshifted emission from the 157.74 mu m [CII] line in the z = 4.4074 quasar BRI 1335-0417. The linewidth and redshift are in good agreement with previous observations of high-J CO line emission. We measure a [CII] line luminosity, L([CII]) = (16.4 +/- 2.6) x 10(9) L(circle dot), making BRI 1335-0417 the most luminous, unlensed [CII] line emitter known at high-redshift. The [CII]-to-FIR luminosity ratio of (5.3 +/- 0.8) x 10(-4) is similar to 3x higher than expected for an average object with a FIR luminosity L(FIR) = 3.1 x 10(13) L(circle dot), if this ratio were to follow the trend observed in other FIR-bright galaxies that have been detected in [CII] line emission. These new data suggest that the scatter in the [CII]-to-FIR luminosity ratio could be larger than previously expected for high luminosity objects. BR1335-0417 has a similar FIR luminosity and [CII]/CO luminosity compared to local ULIRGS and appears to be a gas-rich merger forming stars at a rate of a few thousand solar masses per year. C1 [Wagg, J.] European So Observ, Santiago 19, Chile. [Carilli, C. L.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cox, P.] Inst Radioastron Millimetr, F-38406 St Martin Dheres, France. [De Breuck, C.] European So Observ, D-85748 Garching, Germany. [Menten, K.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Riechers, D. A.] CALTECH, Pasadena, CA 91125 USA. [Walter, F.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Wagg, J (reprint author), European So Observ, Casilla 19001, Santiago 19, Chile. EM jwagg@eso.org OI De Breuck, Carlos/0000-0002-6637-3315 FU NASA [HST-HF-51235.01, NAS 5-26555] FX We thank the staff of the APEX telescope for help with the observations and data analysis. In particular we thank Thomas Stanke, Andreas Lundgren, Rodrigo Parra, Francisco Montenegro, Giorgio Siringo, and Claudio Agurto. D. R. acknowledges support from from NASA through Hubble Fellowship grant HST-HF-51235.01 awarded by STScI, operated by AURA for NASA, under contract NAS 5-26555. We thank the referee for useful comments and suggestions on the manuscript. NR 27 TC 37 Z9 37 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2010 VL 519 AR L1 DI 10.1051/0004-6361/201015424 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 668UQ UT WOS:000283297300118 ER PT J AU Gonzalez, AH Papovich, C Bradac, M Jones, C AF Gonzalez, Anthony H. Papovich, Casey Bradac, Marusa Jones, Christine TI SPECTROSCOPIC CONFIRMATION OF A z=2.79 MULTIPLY IMAGED LUMINOUS INFRARED GALAXY BEHIND THE BULLET CLUSTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: high-redshift; galaxies: starburst; gravitational lensing: strong ID STAR-FORMING GALAXIES; LYMAN BREAK GALAXY; AROMATIC-HYDROCARBON EMISSION; SPITZER-SPACE-TELESCOPE; INITIAL MASS FUNCTION; MIDINFRARED SPECTROSCOPY; REDSHIFT Z-SIMILAR-TO-2; SUBMILLIMETER GALAXIES; DUST; EVOLUTION AB We report spectroscopic confirmation and high-resolution infrared imaging of a z = 2.79 triply imaged galaxy behind the Bullet Cluster. This source, a Spitzer-selected luminous infrared galaxy, is confirmed via polycyclic aromatic hydrocarbon (PAH) features using the Spitzer Infrared Spectrograph (IRS) and resolved with Hubble Space Telescope Wide Field Camera 3 imaging. In this galaxy, which with a stellar mass M* approximate to 4 x 10(9) M(circle dot) is one of the two least massive ones studied with IRS at z > 2, we also detect H(2) S(4) and H(2) S(5) pure rotational lines (at 3.1 sigma and 2.1 sigma)-the first detection of these molecular hydrogen lines in a high-redshift galaxy. From the molecular hydrogen lines we infer an excitation temperature T = 377(-84)(+68) K. The detection of these lines indicates that the warm molecular gas mass is 6(-4)(+346)% of the stellar mass and implies the likely existence of a substantial reservoir of cold molecular gas in the galaxy. Future spectral observations at longer wavelengths with facilities such as the Herschel Space Observatory, the Large Millimeter Telescope, and the Atacama Pathfinder Experiment thus hold the promise of precisely determining the total molecular gas mass. Given the redshift, and using refined astrometric positions from the high-resolution imaging, we also update the magnification estimate and derived fundamental physical properties of this system. The previously published values for L(IR), star formation rate, and dust temperature are confirmed modulo the revised magnification; however, we find that PAH emission is roughly a factor of 5 stronger than would be predicted by the relations between L(IR) and L(PAH) reported for SMGs and starbursts in Pope et al. C1 [Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Papovich, Casey] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. [Bradac, Marusa] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Jones, Christine] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gonzalez, AH (reprint author), Univ Florida, Dept Astron, Gainesville, FL 32611 USA. EM anthony@astro.ufl.edu FU NASA; NASA/HST [HST-GO-10200, HST-GO-10863, HST-GO-11099]; NASA/Spitzer [1319141, 1376614] FX A.H.G. and C.P. thank Eiichi Egami, Jane Rigby, and Ranga-Ram Chary for constructive discussions related to this work. The authors also thank the anonymous referee for comments that improved this paper. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. The authors acknowledge support for this work from NASA/HST grants HST-GO-10200, HST-GO-10863, and HST-GO-11099, as well as NASA/Spitzer grants 1319141 and 1376614. NR 46 TC 10 Z9 10 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2010 VL 720 IS 1 BP 245 EP 251 DI 10.1088/0004-637X/720/1/245 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DJ UT WOS:000281596000021 ER PT J AU Slane, P Castro, D Funk, S Uchiyama, Y Lemiere, A Gelfand, JD Lemoine-Goumard, M AF Slane, P. Castro, D. Funk, S. Uchiyama, Y. Lemiere, A. Gelfand, J. D. Lemoine-Goumard, M. TI FERMI DETECTION OF THE PULSAR WIND NEBULA HESS J1640-465 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (HESS J1640-465, FGL J1640.8-4634, 3EG J1639-4702, G338.3-0.0); ISM: supernova remnants; pulsars: general ID LARGE-AREA TELESCOPE; GAMMA-RAY EMISSION; SUPERNOVA REMNANT; RX J1713.7-3946; X-RAY; EVOLUTION; ACCELERATION; SPECTRUM; CATALOG; GALAXY AB We present observations of HESS J1640-465 with the Fermi-Large Area Telescope. The source is detected with high confidence as an emitter of high-energy gamma-rays. The spectrum lacks any evidence for the characteristic cutoff associated with emission from pulsars, indicating that the emission arises primarily from the pulsar wind nebula (PWN). Broadband modeling implies an evolved nebula with a low magnetic field resulting in a high gamma-ray to X-ray flux ratio. The Fermi emission exceeds predictions of the broadband model, and has a steeper spectrum, possibly resulting from a distinct excess of low energy electrons similar to what is inferred for both the Vela X and Crab PWNe. C1 [Slane, P.; Castro, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Castro, D.] Univ Simon Bolivar, Dept Fis, Valle De Sartenejas, Venezuela. [Funk, S.; Uchiyama, Y.] Stanford Linear Accelerator Ctr, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94025 USA. [Lemiere, A.] CNRS, IN2P3, Inst Phys Nucl, F-91400 Orsay, France. [Gelfand, J. D.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Lemoine-Goumard, M.] Univ Bordeaux, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan,UMR 5797, F-33175 Gradignan, France. RP Slane, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM slane@cfa.harvard.edu; dcastro@head.cfa.harvard.edu; funk@slac.stanford.edu; uchiyama@slac.stanford.edu RI Funk, Stefan/B-7629-2015; Gelfand, Joseph/F-1110-2015 OI Funk, Stefan/0000-0002-2012-0080; Gelfand, Joseph/0000-0003-4679-1058 FU NASA [NAS8-39073]; Fermi [NNX09AT68G]; NSF [AST-0702957]; INAF in Italy; CNES in France FX The work presented here was supported in part by NASA Contract NAS8-39073 (P.O.S.) and Fermi Grant NNX09AT68G. J.D.G. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-0702957. P.O.S., S.F., and Y.U. are grateful to the KITP in Santa Barbara, where elements of the work presented here were first discussed during a KITP program. The authors thank Don Ellison, Luke Drury, Felix Aharonian, and David Smith for helpful discussions during the preparation of this paper.; The Fermi-LAT Collaboration acknowledges support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in Italy, MEXT, KEK, and JAXA in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the National Space Board in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged. NR 35 TC 33 Z9 33 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2010 VL 720 IS 1 BP 266 EP 271 DI 10.1088/0004-637X/720/1/266 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DJ UT WOS:000281596000024 ER PT J AU Mancone, CL Gonzalez, AH Brodwin, M Stanford, SA Eisenhardt, PRM Stern, D Jones, C AF Mancone, Conor L. Gonzalez, Anthony H. Brodwin, Mark Stanford, Spencer A. Eisenhardt, Peter R. M. Stern, Daniel Jones, Christine TI THE FORMATION OF MASSIVE CLUSTER GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: evolution galaxies: formation; galaxies: luminosity function, mass function ID IRAC SHALLOW SURVEY; STELLAR POPULATION SYNTHESIS; NEAR-INFRARED PROPERTIES; LUMINOSITY FUNCTION; RED SEQUENCE; STAR-FORMATION; EVOLUTION; SPITZER; 1ST; UNCERTAINTIES AB We present composite 3.6 and 4.5 mu m luminosity functions (LFs) for cluster galaxies measured from the Spitzer Deep, Wide-Field Survey for 0.3 < z < 2. We compare the evolution of m* for these LFs to models for passively evolving stellar populations to constrain the primary epoch of star formation in massive cluster galaxies. At low redshifts (z less than or similar to 1.3), our results agree well with models with no mass assembly and passively evolving stellar populations with a luminosity-weighted mean formation redshift z(f) = 2.4 assuming a Kroupa initial mass function (IMF). We conduct a thorough investigation of systematic biases that might influence our results, and estimate systematic uncertainties of Delta z(f) = (+0.16)(-0.18) (model normalization), Delta z(f) = (+0.40)(-0.05) (a), and Delta z(f) = (+0.30)(-0.45) (choice of stellar population model). For a Salpeter-type IMF, the typical formation epoch is thus strongly constrained to be z similar to 2-3. Higher formation redshifts can only be made consistent with the data if one permits an evolving IMF that is bottom-light at high redshift, as suggested by van Dokkum. At high redshifts (z greater than or similar to 1.3), we also witness a statistically significant (>5 sigma) disagreement between the measured LF and the continuation of the passive evolution model from lower redshifts. After considering potential systematic biases that might influence our highest redshift data points, we interpret the observed deviation as potential evidence for ongoing mass assembly at this epoch. C1 [Mancone, Conor L.; Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Brodwin, Mark; Jones, Christine] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stanford, Spencer A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Stanford, Spencer A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [Eisenhardt, Peter R. M.; Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mancone, CL (reprint author), Univ Florida, Dept Astron, Gainesville, FL 32611 USA. EM cmaneone@astro.ufl.edu; anthony@astro.ufl.edu FU National Science Foundation [AST-0708490]; U.S. Department of Energy by Lawrence Livermore National Laboratory [W-7405-Eng-48, DE-AC52-07NA27344]; NASA FX This paper is based upon work supported by the National Science Foundation under grant AST-0708490. Part of this work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory in part under Contract W-7405-Eng-48 and in part under Contract DE-AC52-07NA27344. The work of P.R.M.E. and D.S. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 40 TC 46 Z9 46 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2010 VL 720 IS 1 BP 284 EP 298 DI 10.1088/0004-637X/720/1/284 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DJ UT WOS:000281596000026 ER PT J AU Oberg, KI Qi, CH Fogel, JKJ Bergin, EA Andrews, SM Espaillat, C van Kempen, TA Wiener, DJ Pascucci, I AF Oberg, Karin I. Qi, Chunhua Fogel, Jeffrey K. J. Bergin, Edwin A. Andrews, Sean M. Espaillat, Catherine van Kempen, Tim A. Wiener, David J. Pascucci, Ilaria TI THE DISK IMAGING SURVEY OF CHEMISTRY WITH SMA. I. TAURUS PROTOPLANETARY DISK DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: molecules; protoplanetary disks; radio lines: ISM; stars: formation; techniques: high angular resolution ID HERBIG-AE STARS; INTERMEDIATE-MASS STARS; T-TAURI; CIRCUMSTELLAR DISKS; HIGH-RESOLUTION; GM-AURIGAE; DM-TAURI; DEUTERATED MOLECULES; TRANSITIONAL DISKS; ACCRETION RATES AB Chemistry plays an important role in the structure and evolution of protoplanetary disks, with implications for the composition of comets and planets. This is the first of a series of papers based on data from DISCS, a Submillimeter Array survey of the chemical composition of protoplanetary disks. The six Taurus sources in the program (DM Tau, AA Tau, LkCa 15, GM Aur, CQ Tau, and MWC 480) range in stellar spectral type from M1 to A4 and offer an opportunity to test the effects of stellar luminosity on the disk chemistry. The disks were observed in 10 different lines at similar to 3" resolution and an rms of similar to 100 mJy beam(-1) at similar to 0.5 km s(-1). The four brightest lines are CO 2-1, HCO(+) 3-2, CN 2(33/4/2) - 1(22/3/1), and HCN 3-2, and these are detected toward all sources (except for HCN toward CQ Tau). The weaker lines of CN 2(22)-1(11), DCO(+) 3-2, N(2)H(+) 3-2, H(2)CO 3(03)-2(02), and 4(14)-3(13) are detected toward two to three disks each, and DCN 3-2 only toward LkCa 15. CH(3)OH 4(21)-3(12) and c-C(3)H(2) are not detected. There is no obvious difference between the T Tauri and Herbig Ae sources with regard to CN and HCN intensities. In contrast, DCO(+), DCN, N(2)H(+), and H(2)CO are detected only toward the T Tauri stars, suggesting that the disks around Herbig Ae stars lack cold regions for long enough timescales to allow for efficient deuterium chemistry, CO freeze-out, and grain chemistry. C1 [Oberg, Karin I.; Qi, Chunhua; Andrews, Sean M.; Espaillat, Catherine; van Kempen, Tim A.; Wiener, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fogel, Jeffrey K. J.; Bergin, Edwin A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Pascucci, Ilaria] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Oberg, KI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA [NAS 5-26555]; National Science Foundation [0901947, 0707777]; Smithsonian Institution; Academia Sinica FX This work has benefited from discussions with and comments from Ewine van Dishoeck, Geoffrey Blake, and Michiel Hogerheijde, and from a helpful review by an anonymous referee. The SMA is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. Support for K.I.O. and S.M.A. is provided by NASA through Hubble Fellowship grants awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. C.E. was supported by the National Science Foundation under Award No. 0901947. E.A.B. acknowledges support from NSF Grant 0707777. NR 84 TC 60 Z9 60 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2010 VL 720 IS 1 BP 480 EP 493 DI 10.1088/0004-637X/720/1/480 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DJ UT WOS:000281596000040 ER PT J AU Liu, GC Birkinshaw, M Wu, JHP Ho, PTP Huang, CWL Liao, YW Lin, KY Molnar, SM Nishioka, H Koch, PM Umetsu, K Wang, FC Altamirano, P Chang, CH Chang, SH Chang, SW Chen, MT Han, CC Huang, YD Hwang, YJ Jiang, HM Kesteven, M Kubo, D Li, CT Martin-Cocher, P Oshiro, P Raffin, P Wei, T Wilson, W AF Liu, Guo-Chin Birkinshaw, Mark Wu, Jiun-Huei Proty Ho, Paul T. P. Huang, Chih-Wei Locutus Liao, Yu-Wei Lin, Kai-Yang Molnar, Sandor M. Nishioka, Hiroaki Koch, Patrick M. Umetsu, Keiichi Wang, Fu-Cheng Altamirano, Pablo Chang, Ciia-Hao Chang, Shu-Hao Chang, Su-Wei Chen, Ming-Tang Han, Chih-Chiang Huang, Yau-De Hwang, Yuh-Jing Jiang, Homin Kesteven, Michael Kubo, Derek Li, Chao-Te Martin-Cocher, Pierre Oshiro, Peter Raffin, Philippe Wei, Tashun Wilson, Warwick TI CONTAMINATION OF THE CENTRAL SUNYAEV-ZEL'DOVICH DECREMENTS IN AMiBA GALAXY CLUSTER OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; diffuse radiation; galaxies: clusters: general ID MICROWAVE BACKGROUND ANISOTROPY; RADIO-SOURCES; SCALING RELATIONS; SOURCE CATALOG; X-RAY; ARRAY; MASS; CMB AB We investigate the contamination of the Sunyaev-Zel'dovich (SZ) effect for six galaxy clusters, A1689, A1995, A2142, A2163, A2261, and A2390, observed by the Y. T. Lee Array for Microwave Background Anisotropy in 2007. With the range of baselines used, we find that the largest effect (of order 13%-50% of the central SZ flux density) comes from primary anisotropies in the cosmic microwave background and exceeds the thermal noise in all six cases. Contamination from discrete radio sources is estimated to be at a level of 3%-60% of the central SZ flux density. We use the statistics of these contaminating sources to estimate and correct the errors in the measured SZ effects of these clusters. C1 [Liu, Guo-Chin; Ho, Paul T. P.; Lin, Kai-Yang; Molnar, Sandor M.; Nishioka, Hiroaki; Koch, Patrick M.; Umetsu, Keiichi; Altamirano, Pablo; Chang, Ciia-Hao; Chang, Shu-Hao; Chang, Su-Wei; Chen, Ming-Tang; Han, Chih-Chiang; Huang, Yau-De; Hwang, Yuh-Jing; Jiang, Homin; Kubo, Derek; Li, Chao-Te; Martin-Cocher, Pierre; Oshiro, Peter; Raffin, Philippe; Wei, Tashun] Inst Astron & Astrophys, Acad Sinica, Taipei 106, Taiwan. [Liu, Guo-Chin] Tamkang Univ, Dept Phys, Tamsui 25137, Taipei County, Taiwan. [Birkinshaw, Mark] Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. [Wu, Jiun-Huei Proty; Huang, Chih-Wei Locutus; Liao, Yu-Wei; Lin, Kai-Yang; Wang, Fu-Cheng] Natl Taiwan Univ, Dept Phys, Inst Astrophys, Taipei 10617, Taiwan. [Wu, Jiun-Huei Proty; Huang, Chih-Wei Locutus; Liao, Yu-Wei; Lin, Kai-Yang; Wang, Fu-Cheng] Natl Taiwan Univ, Ctr Theoret Sci, Taipei 10617, Taiwan. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kesteven, Michael; Wilson, Warwick] Australia Telescope Natl Facil, Epping, NSW 1710, Australia. RP Liu, GC (reprint author), Inst Astron & Astrophys, Acad Sinica, POB 23-141, Taipei 106, Taiwan. OI WU, JIUN-HUEI/0000-0001-9608-7662; Umetsu, Keiichi/0000-0002-7196-4822 FU STFC; National Science Council of Taiwan [NSC97-2112-M-032-007-MY3, NSC97-2112-M-001-020-MY3] FX We acknowledge the extensive use we have made of data from the WMAP satellite, and thank Dr. L. Chiang for fruitful discussions on Galactic emission and the WMAP data. We also appreciate discussions with Drs. N. Aghanim and S. Matsushita on radio source properties. Support from the STFC for MB is acknowledged. This work is partially supported by the National Science Council of Taiwan under grants NSC97-2112-M-032-007-MY3 and NSC97-2112-M-001-020-MY3. NR 31 TC 4 Z9 4 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2010 VL 720 IS 1 BP 608 EP 613 DI 10.1088/0004-637X/720/1/608 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DJ UT WOS:000281596000052 ER PT J AU Espada, D Peck, AB Matsushita, S Sakamoto, K Henkel, C Iono, D Israel, FP Muller, S Petitpas, G Pihlstrom, Y Taylor, GB Trung, DV AF Espada, D. Peck, A. B. Matsushita, S. Sakamoto, K. Henkel, C. Iono, D. Israel, F. P. Muller, S. Petitpas, G. Pihlstrom, Y. Taylor, G. B. Trung, D. V. TI DISENTANGLING THE CIRCUMNUCLEAR ENVIRONS OF CENTAURUS A. II. ON THE NATURE OF THE BROAD ABSORPTION LINE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: individual (NGC 5128); galaxies: ISM; galaxies: structure; quasars: absorption lines ID NUCLEAR STARBURST ENVIRONMENT; H-I ABSORPTION; MOLECULAR ABSORPTION; RADIO GALAXY; NEARBY GALAXIES; CARBON-MONOXIDE; SCALE STRUCTURE; DENSE GAS; NGC 5128; EMISSION AB We report on atomic gas (Hi) and molecular gas (as traced by CO(2-1)) redshifted absorption features toward the nuclear regions of the closest powerful radio galaxy, Centaurus A (NGC 5128). Our Hi observations using the Very Long Baseline Array allow us to discern with unprecedented sub-parsec resolution Hi absorption profiles toward different positions along the 21 cm continuum jet in the inner 0 ''.3 (or 5.4 pc). In addition, our CO(2-1) data obtained with the Submillimeter Array probe the bulk of the absorbing molecular gas with little contamination by emission, which was not possible with previous CO single-dish observations. We shed light on the physical properties of the gas in the line of sight with these data, emphasizing the still open debate about the nature of the gas that produces the broad absorption line (similar to 55 km s(-1)). First, the broad Hi line is more prominent toward the central and brightest 21 cm continuum component than toward a region along the jet at a distance similar to 20 mas (or 0.4 pc) further from the nucleus. This indicates that the broad absorption line arises from gas located close to the nucleus, rather than from diffuse and more distant gas. Second, the different velocity components detected in the CO(2-1) absorption spectrum match well with other molecular lines, such as those of HCO(+)(1-0), except the broad absorption line that is detected in HCO(+)(1-0) (and most likely related to that of the HI). Dissociation of molecular hydrogen due to the active galactic nucleus seems to be efficient at distances r less than or similar to 10 pc, which might contribute to the depth of the broad Hi and molecular lines. C1 [Espada, D.; Matsushita, S.; Sakamoto, K.; Trung, D. V.] Inst Astron & Astrophys, Acad Sinica, Taipei 10617, Taiwan. [Espada, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Espada, D.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Peck, A. B.; Matsushita, S.] Joint ALMA Off, Santiago, Chile. [Peck, A. B.; Petitpas, G.] Harvard Smithsonian Ctr Astrophys, Hilo, HI 96720 USA. [Peck, A. B.; Pihlstrom, Y.; Taylor, G. B.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Henkel, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Iono, D.] NAOJ, Nobeyama Radio Observ, Minamimaki, Nagano 3841305, Japan. [Israel, F. P.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. [Muller, S.] Onsala Space Observ, SE-43992 Onsala, Sweden. [Pihlstrom, Y.; Taylor, G. B.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Trung, D. V.] Vietnam Acad Sci & Technol, Ctr Quantum Elect, Inst Phys, Hanoi, Vietnam. RP Espada, D (reprint author), Inst Astron & Astrophys, Acad Sinica, POB 23-141, Taipei 10617, Taiwan. EM despada@cfa.harvard.edu OI /0000-0002-9931-1313 FU National Aeronautics and Space Administration; European Community [MOIF-CT-2006-40298] FX We thank the SMA and NRAO staff members who made the observations reported here possible. We also thank A. Sarma for providing the 21 cm continuum VLA data, and S. Martin and I. Jimenez-Serra for interesting discussions. This research has made use of NASA's Astrophysics Data System Bibliographic Services and has also made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. D.E. was supported by a Marie Curie International Fellowship within the 6th European Community Framework Programme (MOIF-CT-2006-40298). NR 51 TC 10 Z9 10 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2010 VL 720 IS 1 BP 666 EP 678 DI 10.1088/0004-637X/720/1/666 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DJ UT WOS:000281596000058 ER PT J AU Beerer, IM Koenig, XP Hora, JL Gutermuth, RA Bontemps, S Megeath, ST Schneider, N Motte, F Carey, S Simon, R Keto, E Smith, HA Allen, LE Fazio, GG Kraemer, KE Price, S Mizuno, D Adams, JD Hernandez, J Lucas, PW AF Beerer, I. M. Koenig, X. P. Hora, J. L. Gutermuth, R. A. Bontemps, S. Megeath, S. T. Schneider, N. Motte, F. Carey, S. Simon, R. Keto, E. Smith, H. A. Allen, L. E. Fazio, G. G. Kraemer, K. E. Price, S. Mizuno, D. Adams, J. D. Hernandez, J. Lucas, P. W. TI A SPITZER VIEW OF STAR FORMATION IN THE CYGNUS X NORTH COMPLEX SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: stars; H II regions; stars: early-type; stars: formation; stars: pre-main sequence ID GALACTIC PLANE IPHAS; H-ALPHA SURVEY; MOLECULAR CLOUD; OB ASSOCIATIONS; SPACE-TELESCOPE; CLUSTER; REGION; 2MASS; SKY; SPECTROGRAPH AB We present new images and photometry of the massive star-forming complex Cygnus X obtained with the Infrared Array Camera (IRAC) and the Multiband Imaging Photometer for Spitzer (MIPS) on board the Spitzer Space Telescope. A combination of IRAC, MIPS, UKIRT Deep Infrared Sky Survey, and Two Micron All Sky Survey data are used to identify and classify young stellar objects (YSOs). Of the 8231 sources detected exhibiting infrared excess in Cygnus X North, 670 are classified as class I and 7249 are classified as class II. Using spectra from the FAST Spectrograph at the Fred L. Whipple Observatory and Hectospec on the MMT, we spectrally typed 536 sources in the Cygnus X complex to identify the massive stars. We find that YSOs tend to be grouped in the neighborhoods of massive B stars (spectral types B0 to B9). We present a minimal spanning tree analysis of clusters in two regions in Cygnus X North. The fraction of infrared excess sources that belong to clusters with >= 10 members is found to be 50%-70%. Most class II objects lie in dense clusters within blown out H II regions, while class I sources tend to reside in more filamentary structures along the bright-rimmed clouds, indicating possible triggered star formation. C1 [Beerer, I. M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Koenig, X. P.; Hora, J. L.; Keto, E.; Smith, H. A.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gutermuth, R. A.] Smith Coll, Northampton, MA 01063 USA. [Gutermuth, R. A.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Bontemps, S.; Schneider, N.] Observ Bordeaux, F-33270 Floirac, France. [Megeath, S. T.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Motte, F.] CEA Saclay, AIM SAp, F-91191 Gif Sur Yvette, France. [Carey, S.] Spitzer Sci Ctr, Pasadena, CA USA. [Simon, R.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Allen, L. E.] Natl Opt Astron Observ, Tucson, AZ USA. [Kraemer, K. E.; Price, S.] USAF, Res Lab, Hanscom AFB, MA USA. [Mizuno, D.] Boston Coll, Inst Sci Res, Boston, MA USA. [Adams, J. D.] Cornell Univ, Dept Radiophys Space Res, Ithaca, NY USA. [Hernandez, J.] Ctr Invest Astron, Merida 5101 A, Venezuela. [Lucas, P. W.] Univ Hertfordshire, Ctr Astrophys Res, Harefield, Middx, England. [Lucas, P. W.] Univ Hertfordshire, Sci & Technol Res Inst, Harefield, Middx, England. RP Beerer, IM (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. OI Koenig, Xavier/0000-0002-9478-4170; Hora, Joseph/0000-0002-5599-4650; Kraemer, Kathleen/0000-0002-2626-7155 FU NASA; National Science Foundation; Department of Defense [0754568]; Smithsonian Institution FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. This work was supported in part by the National Science Foundation Research Experiences for Undergraduates (REU) and Department of Defense Awards to Stimulate and Support Undergraduate Research Experiences (ASSURE) programs under grant No. 0754568 and by the Smithsonian Institution. NR 54 TC 22 Z9 22 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2010 VL 720 IS 1 BP 679 EP 693 DI 10.1088/0004-637X/720/1/679 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DJ UT WOS:000281596000059 ER PT J AU McClelland, CM Garnavich, PM Galbany, L Miquel, R Foley, RJ Filippenko, AV Bassett, B Wheeler, JC Goobar, A Jha, SW Sako, M Frieman, JA Sollerman, J Vinko, J Schneider, DP AF McClelland, Colin M. Garnavich, Peter M. Galbany, Lluis Miquel, Ramon Foley, Ryan J. Filippenko, Alexei V. Bassett, Bruce Wheeler, J. Craig Goobar, Ariel Jha, Saurabh W. Sako, Masao Frieman, Joshua A. Sollerman, Jesper Vinko, Jozsef Schneider, Donald P. TI THE SUBLUMINOUS SUPERNOVA 2007qd: A MISSING LINK IN A FAMILY OF LOW-LUMINOSITY TYPE Ia SUPERNOVAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (SDSS J020932.73-005959.8); supernovae: general; supernovae: individual (SN 2007qd, SN 2008ha, SN 2002cx, SN 2005hk) ID DIGITAL SKY SURVEY; LIGHT-CURVE SHAPES; HUBBLE-SPACE-TELESCOPE; SN 2008HA; MODELS; CONSTANT; CONSTRAINTS; PROGENITOR; DISTANCE; SPECTRA AB We present multi-band photometry and multi-epoch spectroscopy of the peculiar Type Ia supernova (SN la) 2007qd, discovered by the SDSS-II Supernova Survey. It possesses physical properties intermediate to those of the peculiar SN 2002cx and the extremely low-luminosity SN 2008ha. Optical photometry indicates that it had an extraordinarily fast rise time of less than or similar to 10 days and a peak absolute B magnitude of -15.4 +/- 0.2 at most, making it one of the most subluminous SN la ever observed. Follow-up spectroscopy of SN 2007qd near maximum brightness unambiguously shows the presence of intermediate-mass elements which are likely caused by carbon/oxygen nuclear burning. Near maximum brightness, SN 2007qd had a photospheric velocity of only 2800 km s(-1), similar to that of SN 2008ha but about 4000 and 7000 km s(-1) less than that of SN 2002cx and normal SN la, respectively. We show that the peak luminosities of SN 2002cx like objects are highly correlated with both their light-curve stretch and photospheric velocities. Its strong apparent connection to other SN 2002cx like events suggests that SN 2007qd is also a pure deflagration of a white dwarf, although other mechanisms cannot be ruled out. It may be a critical link between SN 2008ha and the other members of the SN 2002cx like class of objects. C1 [McClelland, Colin M.; Garnavich, Peter M.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Galbany, Lluis; Miquel, Ramon] Univ Autonoma Barcelona, Inst Fis Altes Energies, E-08193 Barcelona, Spain. [Miquel, Ramon] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Foley, Ryan J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Bassett, Bruce] Univ Cape Town, Dept Math & Appl Math, ZA-7701 Rondebosch, South Africa. [Wheeler, J. Craig] Univ Texas Austin, Dept Astron, McDonald Observ, Austin, TX 78712 USA. [Goobar, Ariel] Stockholm Univ, Dept Phys, AlbaNova Univ Ctr, SE-10691 Stockholm, Sweden. [Goobar, Ariel] Stockholm Univ, Dept Phys, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Jha, Saurabh W.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Sako, Masao] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Frieman, Joshua A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Frieman, Joshua A.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Frieman, Joshua A.] Fermilab Natl Accelerator Lab, Ctr Particle Astrophys, Batavia, IL 60510 USA. [Sollerman, Jesper] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Sollerman, Jesper] Stockholm Univ, Dept Astron, Oskar Klein Ctr, S-10691 Stockholm, Sweden. [Vinko, Jozsef] Univ Szeged, Dept Opt & Quantum Elect, Szeged, Hungary. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP McClelland, CM (reprint author), Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. RI Galbany, Lluis/A-8963-2017; OI Galbany, Lluis/0000-0002-1296-6887; Bassett, Bruce/0000-0001-7700-1069; Sollerman, Jesper/0000-0003-1546-6615; Vinko, Jozsef/0000-0001-8764-7832; Miquel, Ramon/0000-0002-6610-4836 FU Alfred P. Sloan Foundation; National Science Foundation (NSF) [AST-0908886, AST-0847157]; U.S. Department of Energy (DOE); National Aeronautics and Space Administration (NASA); Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences; Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington; W. M. Keck Foundation; University of Notre Dame; NASA/STScI [HST-GO-10893.01-A]; DOE [DE-FG02-08ER41563, DE-FG02-08ER41562] FX Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation (NSF), the U.S. Department of Energy (DOE), the National Aeronautics and Space Administration (NASA), the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England.; The SDSS Web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.; Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; it was made possible by the generous financial support of the W. M. Keck Foundation. The authors recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community; we are most fortunate to have the opportunity to conduct observations from this mountain. We thank the Keck staff for their assistance.; We are grateful for the financial support of the University of Notre Dame, NASA/STScI Grant HST-GO-10893.01-A to C.M.M., the NSF, and the DOE, specifically NSF grant AST-0908886 and DOE grant DE-FG02-08ER41563 to A.V.F. Support for this research at Rutgers University was provided by DOE grant DE-FG02-08ER41562 and NSF award AST-0847157 to S.W.J. We thank Brian Hayden, Joe Gallagher, and Weidong Li for discussions and their help in the production of this paper, Jerod Parrent and the Online Supernova Spectrum Archive (SUSPECT), and David Jeffery along with the SUSPEND database. NR 97 TC 33 Z9 33 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2010 VL 720 IS 1 BP 704 EP 716 DI 10.1088/0004-637X/720/1/704 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DJ UT WOS:000281596000061 ER PT J AU Burke, DL Axelrod, T Blondin, S Claver, C Ivezic, Z Jones, L Saha, A Smith, A Smith, RC Stubbs, CW AF Burke, David L. Axelrod, T. Blondin, Stephane Claver, Chuck Ivezic, Zeljko Jones, Lynne Saha, Abhijit Smith, Allyn Smith, R. Chris Stubbs, Christopher W. TI PRECISION DETERMINATION OF ATMOSPHERIC EXTINCTION AT OPTICAL AND NEAR-INFRARED WAVELENGTHS SO ASTROPHYSICAL JOURNAL LA English DT Article DE atmospheric effects; methods: observational; surveys; techniques: photometric ID DIGITAL SKY SURVEY; STANDARD STARS; CALIBRATION; PHOTOMETRY; CATALOG AB The science goals for future ground-based all-sky surveys, such as the Dark Energy Survey, PanSTARRS, and the Large Synoptic Survey Telescope, require calibration of broadband photometry that is stable in time and uniform over the sky to precisions of 1% or better, and absolute calibration of color measurements that are similarly accurate. This performance will need to be achieved with measurements made from multiple images taken over the course of many years, and these surveys will observe in less than ideal conditions. This paper describes a technique to implement a new strategy to directly measure variations of atmospheric transmittance at optical wavelengths and application of these measurements to calibration of ground-based observations. This strategy makes use of measurements of the spectra of a small catalog of bright "probe" stars as they progress across the sky and back-light the atmosphere. The signatures of optical absorption by different atmospheric constituents are recognized in these spectra by their characteristic dependences on wavelength and airmass. State-of-the-art models of atmospheric radiation transport and modern codes are used to accurately compute atmospheric extinction over a wide range of observing conditions. We present results of an observing campaign that demonstrate that correction for extinction due to molecular constituents and aerosols can be done with precisions of a few millimagnitudes with this technique. C1 [Burke, David L.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Axelrod, T.] Univ Arizona, Steward Observ, Tucson, AZ 85718 USA. [Blondin, Stephane] ESO, D-85748 Garching, Germany. [Blondin, Stephane] CNRS, IN2P3, CPPM, F-13288 Marseille 09, France. [Claver, Chuck; Saha, Abhijit] Natl Opt Astron Observ, Tucson, AZ 85718 USA. [Ivezic, Zeljko; Jones, Lynne] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Smith, Allyn] Austin Peay State Univ, Dept Phys & Astron, Clarksville, TN 37044 USA. [Smith, R. Chris] Cerro Tololo Interamer Observ, La Serena, Chile. [Stubbs, Christopher W.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Burke, DL (reprint author), SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. EM daveb@slac.stanford.edu RI Stubbs, Christopher/C-2829-2012 OI Stubbs, Christopher/0000-0003-0347-1724 FU National Science Foundation [9 (AST-0551161), AST-0132798]; Department of Energy [DE-AC02-76SF00515, DE-AC02-98Ch10886, DE-FG02-91ER40, DE-FG02-91ER40677, W-7405-Eng-48] FX This work has been done as part of the design and development activity of the Large Synoptic Survey Telescope (LSST). The LSST is supported by the National Science Foundation under Scientific Program Order No. 9 (AST-0551161) through Cooperative Agreement AST-0132798, and under Department of Energy contracts DE-AC02-76SF00515, DE-AC02-98Ch10886, DE-FG02-91ER40, DE-FG02-91ER40677, and W-7405-Eng-48. Additional funding conies from private donations, in-kind support at Department of Energy laboratories and other LSSTC Institutional Members. NR 29 TC 23 Z9 23 U1 2 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2010 VL 720 IS 1 BP 811 EP 823 DI 10.1088/0004-637X/720/1/811 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DJ UT WOS:000281596000069 ER PT J AU Cranmer, SR Van Ballegooijen, AA AF Cranmer, Steven R. Van Ballegooijen, Adriaan A. TI CAN THE SOLAR WIND BE DRIVEN BY MAGNETIC RECONNECTION IN THE SUN'S MAGNETIC CARPET? SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic fields; magnetohydrodynamics (MHD); plasmas; solar wind; Sun: corona; Sun: photosphere ID CORONAL MASS EJECTIONS; ELEMENTARY HEATING EVENTS; 2 FLUX SOURCES; QUIET SUN; ACTIVE REGIONS; TRANSITION REGION; MAGNETOHYDRODYNAMIC TURBULENCE; CHROMOSPHERIC NETWORK; PHOTOSPHERIC MOTIONS; HINODE OBSERVATIONS AB The physical processes that heat the solar corona and accelerate the solar wind remain unknown after many years of study. Some have suggested that the wind is driven by waves and turbulence in open magnetic flux tubes, and others have suggested that plasma is injected into the open tubes by magnetic reconnection with closed loops. In order to test the latter idea, we developed Monte Carlo simulations of the photospheric "magnetic carpet" and extrapolated the time-varying coronal field. These models were constructed for a range of different magnetic flux imbalance ratios. Completely balanced models represent quiet regions on the Sun and source regions of slow solar wind streams. Highly imbalanced models represent corona] holes and source regions of fast wind streams. The models agree with observed emergence rates, surface flux densities, and number distributions of magnetic elements. Despite having no imposed supergranular motions in the models, a realistic network of magnetic "funnels" appeared spontaneously. We computed the rate at which closed field lines open up (i.e., recycling times for open flux), and we estimated the energy flux released in reconnection events involving the opening up of closed flux tubes. For quiet regions and mixed-polarity coronal holes, these energy fluxes were found to be much lower than that which is required to accelerate the solar wind. For the most imbalanced coronal holes, the energy fluxes may be large enough to power the solar wind, but the recycling times are far longer than the time it takes the solar wind to accelerate into the low corona. Thus, it is unlikely that either the slow or fast solar wind is driven by reconnection and loop-opening processes in the magnetic carpet. C1 [Cranmer, Steven R.; Van Ballegooijen, Adriaan A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cranmer, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM scranmer@cfa.harvard.edu; avanballegooijen@cfa.harvard.edu OI van Ballegooijen, Adriaan/0000-0002-5622-3540 FU National Aeronautics and Space Administration (NASA) [NNX09AB27G] FX The authors gratefully acknowledge Ben Chandran, Phil Isenberg, Terry Gaetz, and the anonymous referee for valuable discussions. This work was supported by the National Aeronautics and Space Administration (NASA) under grant NNX09AB27G to the Smithsonian Astrophysical Observatory. The SOLIS data used in this paper are produced cooperatively by NSF/NSO and NASA/LWS. NR 161 TC 29 Z9 30 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2010 VL 720 IS 1 BP 824 EP 847 DI 10.1088/0004-637X/720/1/824 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DJ UT WOS:000281596000070 ER PT J AU Tullmann, R Plucinsky, PP Gaetz, TJ Slane, P Hughes, JP Harrus, I Pannuti, TG AF Tuellmann, R. Plucinsky, P. P. Gaetz, T. J. Slane, P. Hughes, J. P. Harrus, I. Pannuti, T. G. TI SEARCHING FOR THE PULSAR IN G18.95-1.1: DISCOVERY OF AN X-RAY POINT SOURCE AND ASSOCIATED SYNCHROTRON NEBULA WITH CHANDRA SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: supernova remnants; pulsars: general; X-rays: individual (G18.95-1.1) ID SUPERNOVA REMNANT; RADIO-SOURCE; H I; GALAXY; STARS AB Using the Chandra X-ray Observatory, we have pinpointed the location of a faint X-ray point source (CXOU J182913.1-125113) and an associated diffuse nebula in the composite supernova remnant (SNR) G18.95-1.1. These objects appear to be the long-sought pulsar and its wind nebula. The X-ray spectrum of the point source is best described by an absorbed power-law model with Gamma = 1.6 and an N(H) of similar to 1 x 10(22) cm(-2). This model predicts a relatively low unabsorbed X-ray luminosity of about L(X)(0.5-8.0 keV) similar or equal to 4.1 x 10(31) D(2)(2) erg s(-1), where D(2) is the distance in units of 2 kpc. The best-fit model of the diffuse nebula is a combination of thermal (kT = 0.48 keV) and non-thermal (1.4 <= Gamma <= 1.9) emission. The unabsorbed X-ray luminosity of L(X) similar or equal to 5.4 x 10(33) D(2)(2) erg s(-1) in the 0.5-8 keV energy band seems to be largely dominated by the thermal component from the SNR, providing 87% of L(X) in this band. No radio or X-ray pulsations have been reported for CXOU J182913.1-125113. If we assume an age of similar to 5300 yr for G18.95-1.1 and use the X-ray luminosity for the pulsar and the wind nebula together with the relationship between spin-down luminosity (via magnetic dipole radiation) and period, we estimate the pulsar's period to be P similar or equal to 0.4 s. Compared to other rotation-powered pulsars, a magnetic field of 2.2 x 10(13) G is implied by its location in the P-(P) over dot diagram, a value which is close to that of the quantum critical field. C1 [Tuellmann, R.; Plucinsky, P. P.; Gaetz, T. J.; Slane, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hughes, J. P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Harrus, I.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Pannuti, T. G.] Morehead State Univ, Ctr Space Sci, Morehead, KY 40351 USA. RP Tullmann, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rtuellmann@cfa.harvard.edu FU NASA [GO9-0081X] FX Support for this work was provided by NASA through Chandra Award Number GO9-0081X. NR 21 TC 2 Z9 2 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2010 VL 720 IS 1 BP 848 EP 852 DI 10.1088/0004-637X/720/1/848 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647DJ UT WOS:000281596000071 ER PT J AU Gezari, S Rest, A Huber, ME Narayan, G Forster, K Neill, JD Martin, DC Valenti, S Smartt, SJ Chornock, R Berger, E Soderberg, AM Mattila, S Kankare, E Burgett, WS Chambers, KC Dombeck, T Grav, T Heasley, JN Hodapp, KW Jedicke, R Kaiser, N Kudritzki, R Luppino, G Lupton, RH Magnier, EA Monet, DG Morgan, JS Onaka, PM Price, PA Rhoads, PH Siegmund, WA Stubbs, CW Tonry, JL Wainscoat, RJ Waterson, MF Wynn-Williams, CG AF Gezari, S. Rest, A. Huber, M. E. Narayan, G. Forster, K. Neill, J. D. Martin, D. C. Valenti, S. Smartt, S. J. Chornock, R. Berger, E. Soderberg, A. M. Mattila, S. Kankare, E. Burgett, W. S. Chambers, K. C. Dombeck, T. Grav, T. Heasley, J. N. Hodapp, K. W. Jedicke, R. Kaiser, N. Kudritzki, R. Luppino, G. Lupton, R. H. Magnier, E. A. Monet, D. G. Morgan, J. S. Onaka, P. M. Price, P. A. Rhoads, P. H. Siegmund, W. A. Stubbs, C. W. Tonry, J. L. Wainscoat, R. J. Waterson, M. F. Wynn-Williams, C. G. TI GALEX AND PAN-STARRS1 DISCOVERY OF SN IIP 2010aq: THE FIRST FEW DAYS AFTER SHOCK BREAKOUT IN A RED SUPERGIANT STAR SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE supernovae: individual (SN 2010aq); surveys; ultraviolet: general ID CORE-COLLAPSE SUPERNOVAE; FORMING GALAXIES; P SUPERNOVAE; LIGHT CURVES; GRB-060218; SPECTROSCOPY; PROGENITORS; ABUNDANCES; EMISSION; PLATEAU AB We present the early UV and optical light curve of Type IIP supernova (SN) 2010aq at z = 0.0862, and compare it to analytical models for thermal emission following SN shock breakout in a red supergiant star. SN 2010aq was discovered in joint monitoring between the Galaxy Evolution Explorer (GALEX) Time Domain Survey (TDS) in the NUV and the Pan-STARRS1 Medium Deep Survey (PS1 MDS) in the g, r, i, and z bands. The GALEX and Pan-STARRS1 observations detect the SN less than 1 day after the shock breakout, measure a diluted blackbody temperature of 31,000 +/- 6000 K 1 day later, and follow the rise in the UV/optical light curve over the next 2 days caused by the expansion and cooling of the SN ejecta. The high signal-to-noise ratio of the simultaneous UV and optical photometry allows us to fit for a progenitor star radius of 700 +/- 200R(circle dot), the size of a red supergiant star. An excess in UV emission two weeks after shock breakout compared with SNe well fitted by model atmosphere-code synthetic spectra with solar metallicity is best explained by suppressed line blanketing due to a lower metallicity progenitor star in SN 2010aq. Continued monitoring of PS1 MDS fields by the GALEX TDS will increase the sample of early UV detections of Type II SNe by an order of magnitude and probe the diversity of SN progenitor star properties. C1 [Gezari, S.; Huber, M. E.; Grav, T.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Rest, A.; Narayan, G.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Forster, K.; Neill, J. D.; Martin, D. C.] CALTECH, Pasadena, CA 91125 USA. [Valenti, S.; Smartt, S. J.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Chornock, R.; Berger, E.; Soderberg, A. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mattila, S.; Kankare, E.] Univ Turku, Dept Phys & Astron, Tuorla Observ, FI-21500 Piikkio, Finland. [Mattila, S.] AlbaNova Univ Ctr, Dept Astron, Stockholm Observ, SE-10691 Stockholm, Sweden. [Kankare, E.] Nord Opt Telescope, E-38700 Santa Cruz De La Palma, Spain. [Burgett, W. S.; Chambers, K. C.; Dombeck, T.; Heasley, J. N.; Hodapp, K. W.; Jedicke, R.; Kaiser, N.; Kudritzki, R.; Luppino, G.; Magnier, E. A.; Morgan, J. S.; Onaka, P. M.; Price, P. A.; Rhoads, P. H.; Siegmund, W. A.; Tonry, J. L.; Wainscoat, R. J.; Waterson, M. F.; Wynn-Williams, C. G.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Lupton, R. H.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Monet, D. G.] USN Observ, Flagstaff Stn, Flagstaff, AZ 86001 USA. RP Gezari, S (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. EM suvi@pha.jhu.edu RI Stubbs, Christopher/C-2829-2012; Waterson, Mark/B-7352-2013; OI Stubbs, Christopher/0000-0003-0347-1724; Waterson, Mark/0000-0002-0192-2686; Narayan, Gautham/0000-0001-6022-0484; Chambers, Kenneth /0000-0001-6965-7789 FU NASA through Space Telescope Science Institute [HST-HF-01219.01-A]; NASA [NAS 5-26555] FX S.G. thanks I. Rabinak and E. Nakar for kindly providing their models in the GALEX and PS1 filters, L. Dessart for helpful discussions, and the anonymous referee for useful comments. S. G. was supported by NASA through Hubble Fellowship grant HST-HF-01219.01-A awarded by the Space Telescope Science Institute, which is operated by AURA, Inc., for NASA, under contract NAS 5-26555. The PS1 Surveys have been made possible through the combinations of the Institute for Astronomy at the University of Hawaii, The Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg, and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, the University of Durham, the University of Edinburgh, the Queen's University of Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Network, and the National Central University of Taiwan. We gratefully acknowledge NASA's support for construction, operation, and science analysis for the GALEX mission, developed in cooperation with CNES of France and the Korean MOST. NR 36 TC 25 Z9 25 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 1 PY 2010 VL 720 IS 1 BP L77 EP L81 DI 10.1088/2041-8205/720/1/L77 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647HW UT WOS:000281610100016 ER PT J AU Gnedin, OY Brown, WR Geller, MJ Kenyon, SJ AF Gnedin, Oleg Y. Brown, Warren R. Geller, Margaret J. Kenyon, Scott J. TI THE MASS PROFILE OF THE GALAXY TO 80 kpc SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Galaxy: formation; Galaxy: halo; Galaxy: kinematics and dynamics ID VELOCITY DISPERSION PROFILE; DIGITAL SKY SURVEY; DARK-MATTER HALOS; MILKY-WAY HALO; STELLAR MASS; STRIPE 82; CURVE; SUBSTRUCTURE; CONSTRAINTS; STARS AB The Hypervelocity Star Survey presents the currently largest sample of radial velocity measurements of halo stars out to 80 kpc. We apply spherical Jeans modeling to these data in order to derive the mass profile of the Galaxy. We restrict the analysis to distances larger than 25 kpc from the Galactic center, where the density profile of halo stars is well approximated by a single power law with logarithmic slope between -3.5 and -4.5. With this restriction, we also avoid the complication of modeling a flattened Galactic disk. In the range 25 kpc < r < 80 kpc, the radial velocity dispersion declines remarkably little; a robust measure of its logarithmic slope is between -0.05 and -0.1. The circular velocity profile also declines remarkably little with radius. The allowed range of V(c) (80 kpc) lies between 175 and 231 km s(-1), with the most likely value of 193 km s(-1). Compared with the value at the solar location, the Galactic circular velocity declines by less than 20% over an order of magnitude in radius. Such a flat profile requires a massive and extended dark matter halo. The mass enclosed within 80 kpc is 6.9(-1.2)(+3.0)x10(11) M(circle dot). Our sample of radial velocities is large enough that the biggest uncertainty in the mass is not statistical but systematic, dominated by the density slope and anisotropy of the tracer population. Further progress requires modeling observed data sets within realistic simulations of galaxy formation. C1 [Gnedin, Oleg Y.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Brown, Warren R.; Geller, Margaret J.; Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Gnedin, OY (reprint author), Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. EM ognedin@umich.edu; wbrown@cfa.harvard.edu; mgeller@cfa.harvard.edu; skenyon@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X; Gnedin, Oleg/0000-0001-9852-9954 FU NSF [AST-0708087] FX We thank Hans-Walter Rix for clarifying discussions and the organizers of the Sixth Harvard-Smithsonian Sackler Conference, where this work was completed. O.G. is supported in part by the NSF Grant AST-0708087. NR 21 TC 78 Z9 80 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 1 PY 2010 VL 720 IS 1 BP L108 EP L112 DI 10.1088/2041-8205/720/1/L108 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647HW UT WOS:000281610100022 ER PT J AU Munoz-Jaramillo, A Nandy, D Martens, PCH Yeates, AR AF Munoz-Jaramillo, Andres Nandy, Dibyendu Martens, Petrus C. H. Yeates, Anthony R. TI A DOUBLE-RING ALGORITHM FOR MODELING SOLAR ACTIVE REGIONS: UNIFYING KINEMATIC DYNAMO MODELS AND SURFACE FLUX-TRANSPORT SIMULATIONS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: activity; Sun: dynamo; Sun: interior ID OPEN MAGNETIC-FLUX; MERIDIONAL FLOW; TORSIONAL OSCILLATIONS; DIFFERENTIAL ROTATION; FIELD; CYCLE; TACHOCLINE; EVOLUTION; CIRCULATION; CORONA AB The emergence of tilted bipolar active regions (ARs) and the dispersal of their flux, mediated via processes such as diffusion, differential rotation, and meridional circulation, is believed to be responsible for the reversal of the Sun's polar field. This process (commonly known as the Babcock-Leighton mechanism) is usually modeled as a near-surface, spatially distributed alpha-effect in kinematic mean-field dynamo models. However, this formulation leads to a relationship between polar field strength and meridional flow speed which is opposite to that suggested by physical insight and predicted by surface flux-transport simulations. With this in mind, we present an improved double-ring algorithm for modeling the Babcock-Leighton mechanism based on AR eruption, within the framework of an axisymmetric dynamo model. Using surface flux-transport simulations, we first show that an axisymmetric formulation-which is usually invoked in kinematic dynamo models-can reasonably approximate the surface flux dynamics. Finally, we demonstrate that our treatment of the Babcock-Leighton mechanism through double-ring eruption leads to an inverse relationship between polar field strength and meridional flow speed as expected, reconciling the discrepancy between surface flux-transport simulations and kinematic dynamo models. C1 [Munoz-Jaramillo, Andres; Martens, Petrus C. H.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Nandy, Dibyendu] Indian Inst Sci Educ & Res, Dept Phys Sci, Mohampur 741252, W Bengal, India. [Martens, Petrus C. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Yeates, Anthony R.] Univ Dundee, Div Math, Dundee DD1 4HN, Scotland. RP Munoz-Jaramillo, A (reprint author), Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. EM munoz@solar.physics.montana.edu; dnandi@iiserkol.ac.in; martens@solar.physics.montana.edu; anthony@maths.dundee.ac.uk RI Yeates, Anthony/D-1338-2014; OI Yeates, Anthony/0000-0002-2728-4053; Munoz-Jaramillo, Andres/0000-0002-4716-0840 FU NASA [NNG05GE47G]; Government of India; UK STFC FX We thank Aad van Ballegooijen for useful discussions that were crucial for the development of the algorithm mentioned in Section 4. The computations required for this work were performed using the resources of Montana State University and the Harvard-Smithsonian Center for Astrophysics. We thank Keiji Yoshimura at MSU and Alisdair Davey and Henry (Trae) Winter at the CfA for much appreciated technical support. This research was funded by NASA Living With a Star grant NNG05GE47G and has made extensive use of NASA's Astrophysics Data System. D.N. acknowledges support from the Government of India through the Ramanujan Fellowship. A.R.Y. thanks the UK STFC for financial support. NR 27 TC 25 Z9 25 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 1 PY 2010 VL 720 IS 1 BP L20 EP L25 DI 10.1088/2041-8205/720/1/L20 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 647HW UT WOS:000281610100005 ER PT J AU Raghavan, D McAlister, HA Henry, TJ Latham, DW Marcy, GW Mason, BD Gies, DR White, RJ ten Brummelaar, TA AF Raghavan, Deepak McAlister, Harold A. Henry, Todd J. Latham, David W. Marcy, Geoffrey W. Mason, Brian D. Gies, Douglas R. White, Russel J. ten Brummelaar, Theo A. TI A SURVEY OF STELLAR FAMILIES: MULTIPLICITY OF SOLAR-TYPE STARS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE binaries: general; planetary systems; stars: solar-type; stars: statistics; surveys ID ALL-SKY SURVEY; BROWN DWARF DESERT; EXOPLANET HOST STARS; PROPER-MOTION STARS; SPECTROSCOPIC BINARY ORBITS; ICCD SPECKLE OBSERVATIONS; PHOTOELECTRIC RADIAL-VELOCITIES; LONG-PERIOD COMPANIONS; ADAPTIVE OPTICS SURVEY; RHO-CORONAE-BOREALIS AB We present the results of a comprehensive assessment of companions to solar-type stars. A sample of 454 stars, including the Sun, was selected from the Hipparcos catalog with pi > 40 mas, sigma(pi)/pi < 0.05, 0.5 <= B - V <= 1.0 (similar to F6-K3), and constrained by absolute magnitude and color to exclude evolved stars. These criteria are equivalent to selecting all dwarf and subdwarf stars within 25 pc with V-band flux between 0.1 and 10 times that of the Sun, giving us a physical basis for the term "solar-type." New observational aspects of this work include surveys for (1) very close companions with long-baseline interferometry at the Center for High Angular Resolution Astronomy Array, (2) close companions with speckle interferometry, and (3) wide proper-motion companions identified by blinking multi-epoch archival images. In addition, we include the results from extensive radial-velocity monitoring programs and evaluate companion information from various catalogs covering many different techniques. The results presented here include four new common proper-motion companions discovered by blinking archival images. Additionally, the spectroscopic data searched reveal five new stellar companions. Our synthesis of results from many methods and sources results in a thorough evaluation of stellar and brown dwarf companions to nearby Sun-like stars. The overall observed fractions of single, double, triple, and higher-order systems are 56% +/- 2%, 33% +/- 2%, 8% +/- 1%, and 3% +/- 1%, respectively, counting all confirmed stellar and brown dwarf companions. If all candidate, i.e., unconfirmed, companions identified are found to be real, the percentages would change to 54% +/- 2%, 34% +/- 2%, 9% +/- 2%, and 3% +/- 1%, respectively. Our completeness analysis indicates that only a few undiscovered companions remain in this well-studied sample, implying that the majority (54% +/- 2%) of solar-type stars are single, in contrast to the results of prior multiplicity studies. Our sample is large enough to enable a check of the multiplicity dependence on various physical parameters by analyzing appropriate subsamples. Bluer, more massive stars are seen as more likely to have companions than redder, less massive ones, consistent with the trend seen over the entire spectral range. Systems with larger interaction cross sections, i.e., those with more than two components or long orbital periods, are preferentially younger, suggesting that companions may be stripped over time by dynamical interactions. We confirm the planet-metallicity correlation (i.e., higher metallicity stars are more likely to host planets), but are unable to check it for brown dwarfs due to the paucity of such companions, implying that the brown dwarf desert extends over all separation regimes. We find no correlation between stellar companions and metallicity for B - V < 0.625, but among the redder subset, metal-poor stars ([Fe/H] < -0.3) are more likely to have companions with a 2.4 sigma significance. The orbital-period distribution of companions is unimodal and roughly log normal with a peak and median of about 300 years. The period-eccentricity relation shows the expected circularization for periods below 12 days, caused by tidal forces over the age of the Galaxy, followed by a roughly flat distribution. The mass-ratio distribution shows a preference for like-mass pairs, which occur more frequently in relatively close pairs. The fraction of planet hosts among single, binary, and multiple systems are statistically inditinguishable, suggesting that planets are as likely to form around single stars as they are around components of binary or multiple systems with sufficiently wide separations. This, along with the preference of long orbital periods among stellar systems, increases the space around stars conducive for planet formation, and perhaps life. C1 [Raghavan, Deepak; McAlister, Harold A.; Henry, Todd J.; Gies, Douglas R.; White, Russel J.] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30302 USA. [Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Mason, Brian D.] USN Observ, Washington, DC 20392 USA. [ten Brummelaar, Theo A.] Mt Wilson Observ, CHARA Array, Mt Wilson, CA 91023 USA. RP Raghavan, D (reprint author), Georgia State Univ, Ctr High Angular Resolut Astron, POB 3969, Atlanta, GA 30302 USA. EM raghavan@chara.gsu.edu FU College of Arts and Sciences at Georgia State University; National Science Foundation [AST-0606958, AST-0908253]; U.S. Government [NAGW-2166]; National Aeronautics and Space Administration FX We thank Andy Boden, Bill Cochran, Richard Gray, Roger Griffin, Bill Hartkopf, Artie Hatzes, Elliott Horch, Mike Ireland, Hugh Jones, Davy Kirkpatrick, Dagny Looper, Dimitri Pourbaix, Sam Quinn, Andrei Tokovinin, and Nils Turner for their helpful insights on the nature of some specific systems, and in some instances, for making specific observations at our request and sharing their unpublished results. We acknowledge the insightful comments from an anonymous referee, which resulted in a more robust completion analysis of this survey, improving the confidence in our results. Research at the CHARA Array is supported by the College of Arts and Sciences at Georgia State University and by the National Science Foundation through NSF grants AST-0606958 and AST-0908253. Some of the photometric and spectroscopic observations reported here were carried out under the auspices of the SMARTS (Small and Moderate Aperture Research Telescope System) Consortium, which operates several small telescopes at CTIO. We thank RECONS group members, particularly, Jennifer Winters for reducing photometry data, and Wei-Chun Jao for his insights with some of the analysis. This research has made use of the SIMBAD literature database, operated at CDS, Strasbourg, France, NASA's Astrophysics Data System, and the Washington Double Star Catalog maintained by the U.S. Naval Observatory. This effort used multi-epoch images from the Digitized Sky Survey, which was produced at the Space Telescope Science Institute under U.S. Government grant NAGW-2166, and from the SuperCOSMOS Sky Survey. This publication also made use of data products from the Two Micron All Sky Survey (2MASS), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 215 TC 519 Z9 521 U1 2 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2010 VL 190 IS 1 BP 1 EP 42 DI 10.1088/0067-0049/190/1/1 PG 42 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654WN UT WOS:000282201900001 ER PT J AU Kilic, M Leggett, SK Tremblay, PE von Hippel, T Bergeron, P Harris, HC Munn, JA Williams, KA Gates, E Farihi, J AF Kilic, Mukremin Leggett, S. K. Tremblay, P. -E. von Hippel, Ted Bergeron, P. Harris, Hugh C. Munn, Jeffrey A. Williams, Kurtis A. Gates, Evalyn Farihi, J. TI A DETAILED MODEL ATMOSPHERE ANALYSIS OF COOL WHITE DWARFS IN THE SLOAN DIGITAL SKY SURVEY SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE stars: atmospheres; stars: evolution; white dwarfs ID LUMINOSITY FUNCTION; PHOTOMETRIC ANALYSIS; GALACTIC DISK; HELIUM-ATMOSPHERE; DATA RELEASE; USNO-B; STARS; HALO; CATALOG; DEEP AB We present optical spectroscopy and near-infrared photometry of 126 cool white dwarfs (WDs) in the Sloan Digital Sky Survey (SDSS). Our sample includes high proper motion targets selected using the SDSS and USNOB astrometry and a dozen previously known ultracool WD candidates. Our optical spectroscopic observations demonstrate that a clean selection of large samples of cool WDs in the SDSS (and the SkyMapper, Pan-STARRS, and the Large Synoptic Survey Telescope data sets) is possible using a reduced proper motion diagram and a tangential velocity cut-off (depending on the proper motion accuracy) of 30 km s(-1). Our near-infrared observations reveal eight new stars with significant absorption. We use the optical and near-infrared photometry to perform a detailed model atmosphere analysis. More than 80% of the stars in our sample are consistent with either pure hydrogen or pure helium atmospheres. However, the eight stars with significant infrared absorption and the majority of the previously known ultracool WD candidates are best explained with mixed hydrogen and helium atmosphere models. The age distribution of our sample is consistent with a Galactic disk age of 8 Gyr. A few ultracool WDs may be as old as 12-13 Gyr, but our models have problems matching the spectral energy distributions of these objects. There are only two halo WD candidates in our sample. However, trigonometric parallax observations are required for accurate mass and age determinations and to confirm their membership in the halo. C1 [Kilic, Mukremin] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Leggett, S. K.] Gemini Observ, Hilo, HI 96720 USA. [Tremblay, P. -E.; Bergeron, P.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [von Hippel, Ted] Siena Coll, Dept Phys, Loudonville, NY 12211 USA. [Harris, Hugh C.; Munn, Jeffrey A.] US Naval Observ, Flagstaff Stn, Flagstaff, AZ 86001 USA. [Williams, Kurtis A.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Gates, Evalyn] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Gates, Evalyn] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Farihi, J.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RP Kilic, M (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM mkilic@cfa.harvard.edu OI Leggett, Sandy/0000-0002-3681-2989; Williams, Kurtis/0000-0002-1413-7679; Farihi, Jay/0000-0003-1748-602X FU NASA; Caltech; National Science Foundation [AST-0607480, AST-0602288]; NSERC Canada; FQRNT (Quebec); Gemini Observatory; National Aeronautics and Space Administration, Office of Space Science [NCC 5-538] FX We thank J. Liebert for many useful discussions, Andy Stephens for the derivation of the NIRI nonlinearity correction, and an anonymous referee for useful suggestions. Support for this work was provided by NASA through the Spitzer Space Telescope Fellowship Program, under an award from Caltech. This material is also based on work supported by the National Science Foundation under grants AST-0607480 and AST-0602288 and by the NSERC Canada and by the Fund FQRNT (Quebec). S.K.L.'s research is supported by Gemini Observatory. P. Bergeron is a Cottrell Scholar of Research Corporation for Science Advancement.; The Hobby-Eberly Telescope (HET) is a joint project of the University of Texas at Austin, The Pennsylvania State University, Stanford University, Ludwig-Maximilians-Universitat Munchen, and Georg-August-Universitat Gottingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. The Gemini observatory is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), theNational Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia e Tecnologia (Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). The IRTF is operated by the University of Hawaii under Cooperative Agreement no. NCC 5-538 with the National Aeronautics and Space Administration, Office of Space Science, Planetary Astronomy Program. NR 63 TC 39 Z9 39 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 2010 VL 190 IS 1 BP 77 EP 99 DI 10.1088/0067-0049/190/1/77 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 654WN UT WOS:000282201900004 ER PT J AU Prasifka, JR Bradshaw, JD Boe, AA Lee, D Adamski, D Gray, ME AF Prasifka, Jarrad R. Bradshaw, Jeffrey D. Boe, Arvid A. Lee, DoKyoung Adamski, David Gray, Michael E. TI Symptoms, Distribution and Abundance of the Stem-Boring Caterpillar, Blastobasis repartella (Dietz), in Switchgrass SO BIOENERGY RESEARCH LA English DT Article DE Biofuel; Coleophoridae; Microlepidoptera; Tallgrass prairie; Yield ID BORER LEPIDOPTERA AB A potential pest of switchgrass, Panicum virgatum L., was first detected in South Dakota in 2004, where death of partially emerged leaves was noted in a small proportion of tillers. Similar "dead heart" symptoms were observed in switchgrass in Illinois during 2008 and adults of a stem-boring caterpillar were collected and identified as Blastobasis repartella (Dietz). In 2009, a survey of the central United States was used to estimate the distribution and abundance of this insect. In eight northern states, B. repartella was consistently found in both cultivated plots and natural stands of switchgrass. In four southern states, B. repartella was not detected. However, because symptoms are conspicuous for a short period of time, failure to collect stem-borers on one survey date for each southern location does not necessarily define the limit of distribution for B. repartella. Sampling in four northern states showed the proportion of tillers damaged by B. repartella ranged from 1.0-7.2%. Unlike some caterpillars that feed on native grasses, it appears that the egg-laying behavior of adult moths may preclude the use of prescribed burns as an effective method to suppress this stem-boring caterpillar. As a potential pest of switchgrass planted for biomass production, near-term research needs include refining the geographic distribution of B. repartella, quantifying potential losses of switchgrass biomass, and determining whether switchgrass may be bred for resistance this and other stem-boring insects. C1 [Prasifka, Jarrad R.] Univ Illinois, Energy Biosci Inst, Inst Genom Biol, Urbana, IL 61801 USA. [Adamski, David] Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. [Lee, DoKyoung; Gray, Michael E.] Univ Illinois, Dept Crop Sci, Urbana, IL 61801 USA. [Boe, Arvid A.] S Dakota State Univ, Dept Plant Sci, Brookings, SD 57007 USA. RP Prasifka, JR (reprint author), Univ Illinois, Energy Biosci Inst, Inst Genom Biol, Room 1117, Urbana, IL 61801 USA. EM prasifka@illinois.edu FU Energy Biosciences Institute FX Research funding was provided by the Energy Biosciences Institute. The authors wish to thank a number of people who assisted in locating and surveying field plots of switchgrass; Jerry Roitsch (Bristol, South Dakota), Jim Muir (Texas AgriLife Research), Twain Butler (The Samuel Roberts Noble Foundation), Mike Blazier (Lousiana State University Agricultural Center), Randy King (USDA-NRCS), Ken Moore (Iowa State University), Rob Mitchell (USDA-ARS), Mike Casler (USDA-ARS), John Leif (USDA-NRCS), and Yvonne Lawley (North Dakota State University). NR 13 TC 16 Z9 18 U1 1 U2 10 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1939-1234 J9 BIOENERG RES JI BioEnergy Res. PD SEP PY 2010 VL 3 IS 3 BP 238 EP 242 DI 10.1007/s12155-009-9064-8 PG 5 WC Energy & Fuels; Environmental Sciences SC Energy & Fuels; Environmental Sciences & Ecology GA 637HJ UT WOS:000280807800002 ER PT J AU Kennedy, CM Marra, PP AF Kennedy, Christina M. Marra, Peter P. TI Matrix mediates avian movements in tropical forested landscapes: Inference from experimental translocations SO BIOLOGICAL CONSERVATION LA English DT Article DE Neotropics; Caribbean; Tropical conservation; Connectivity; Dispersal; Homing ID GAP-CROSSING DECISIONS; HABITAT FRAGMENTATION; POSTFLEDGING PERIOD; POPULATION-DYNAMICS; BREEDING DISPERSAL; NONBREEDING SEASON; CORRIDOR USE; BIRDS; PATTERNS; JAMAICA AB Maintaining animal movement in fragmented landscapes depends upon the levels of connectivity among habitat patches, which in turn may depend upon the landscape matrix. Little is known about how the matrix affects dispersal abilities, in part because few experimental tests have been conducted. We experimentally translocated 142 migratory American Redstarts (Setophaga ruticilla) and resident Jamaican Todies (Todus todus) 0.6-4 km from their territories across landscapes fragmented by pen-urban development and bauxite mining and continuous forest. Redstarts returned more rapidly and with greater success than todies across all landscapes, with 95% of redstarts returning in an average of 2.5 days versus 60% of todies in >20 days. Return success was best predicted by translocation distance for redstarts and by sex for todies, with a trend of fewer birds returning when released in bauxite landscapes. Return time was strongly affected by matrix type, with both species returning more rapidly in a forested relative to a bauxite matrix and intermediately in a pen-urban matrix. These findings provide strong experimental evidence that land cover surrounding forested habitat influences species mobility. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Kennedy, Christina M.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Marra, Peter P.] Migratory Bird Center, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. RP Kennedy, CM (reprint author), Univ Maryland, Dept Biol, 3221 Biol Psychol Bldg, College Pk, MD 20742 USA. EM cmk6@umd.edu; marrap@si.edu FU NASA; Fulbright; Washington Explorer's Club; Cosmos Club Foundation; University of Maryland; Smithsonian Institution (James Bond Trust); National Science Foundation FX We thank A. Hayes-Sutton for sharing her knowledge of the study region and for providing logistical field support; S. Franks (NASA Goddard Space Flight Center) for assistance in the object-based land cover classification; S. Schill (The Nature Conservancy) and O. Evelyn (Jamaica Forestry Department) for providing remote sensing imagery and GIS data; and Y. Strong and A. Donaldson (Jamaica National Environment and Planning Agency, NEPA) for granting in-country permits. This manuscript was improved with comments from M. Neel, W. Fagan, and D. Inouye (University of Maryland), T. Ricketts (World Wildlife Fund), and two anonymous reviewers. Fieldwork was directed by C. Kennedy with essential field assistance by C. Samuels, M. Podolsky, H. Davis, M. Beale, and M. White. All work was conducted under applicable permits and approved animal care/use protocols (University of Maryland IACUC protocol #R-06-83 to W.F.F. and C.M.K., Smithsonian National Zoological Park CRC-IACUC proposal #06-25 and Jamaica NEPA Ref. No. 18/27 to P.P.M. and C.M.K.). Research was made possible by the permission of many land owners to access their lands, including the Jamaica Forestry Department, Windalco, Alpart Mining Venture, and Jamalco bauxite mining companies, S&G Road Surfacing Materials Ltd., private farmers and Mandeville citizens. Funding was provided to C.M.K. by NASA Earth System Science Program (Doctoral Fellowship), Fulbright US Scholarship Program, Washington Explorer's Club, Cosmos Club Foundation, and the University of Maryland (Behavior, Ecology, Evolution, and Systematics Graduate Program and an Ann G. Wylie Dissertation Fellowship), and provided to P.P.M. and C.M.K. by the Smithsonian Institution (James Bond Trust) and to P.P.M. by the National Science Foundation. NR 63 TC 26 Z9 26 U1 5 U2 36 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 J9 BIOL CONSERV JI Biol. Conserv. PD SEP PY 2010 VL 143 IS 9 BP 2136 EP 2145 DI 10.1016/j.biocon.2010.05.025 PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 641KW UT WOS:000281125400024 ER PT J AU Nyman, T Vikberg, V Smith, DR Boeve, JL AF Nyman, Tommi Vikberg, Veli Smith, David R. Boeve, Jean-Luc TI How common is ecological speciation in plant-feeding insects? A 'Higher' Nematinae perspective SO BMC EVOLUTIONARY BIOLOGY LA English DT Article ID HOST-PLANT; SYMPATRIC SPECIATION; INTERSPECIFIC INTERACTIONS; PHYLOGENETIC ANALYSIS; GEOGRAPHICAL PATTERN; SAWFLIES HYMENOPTERA; CONVERGENT EVOLUTION; PHYTOPHAGOUS INSECTS; MOLECULAR PHYLOGENY; BEETLES COLEOPTERA AB Background: Ecological speciation is a process in which a transiently resource-polymorphic species divides into two specialized sister lineages as a result of divergent selection pressures caused by the use of multiple niches or environments. Ecology-based speciation has been studied intensively in plant-feeding insects, in which both sympatric and allopatric shifts onto novel host plants could speed up diversification. However, while numerous examples of species pairs likely to have originated by resource shifts have been found, the overall importance of ecological speciation in relation to other, non-ecological speciation modes remains unknown. Here, we apply phylogenetic information on sawflies belonging to the 'Higher' Nematinae (Hymenoptera: Tenthredinidae) to infer the frequency of niche shifts in relation to speciation events. Results: Phylogenetic trees reconstructed on the basis of DNA sequence data show that the diversification of higher nematines has involved frequent shifts in larval feeding habits and in the use of plant taxa. However, the inferred number of resource shifts is considerably lower than the number of past speciation events, indicating that the majority of divergences have occurred by non-ecological allopatric speciation; based on a time-corrected analysis of sister species, we estimate that a maximum of c. 20% of lineage splits have been triggered by a change in resource use. In addition, we find that postspeciational changes in geographic distributions have led to broad sympatry in many species having identical host-plant ranges. Conclusion: Our analysis indicates that the importance of niche shifts for the diversification of herbivorous insects is at present implicitly and explicitly overestimated. In the case of the Higher Nematinae, employing a time correction for sister-species comparisons lowered the proportion of apparent ecology-based speciation events from c. 50-60% to around 20%, but such corrections are still lacking in other herbivore groups. The observed convergent but asynchronous shifting among dominant northern plant taxa in many higher-nematine clades, in combination with the broad overlaps in the geographic distributions of numerous nematine species occupying near-identical niches, indicates that host-plant shifts and herbivore community assembly are largely unconstrained by direct or indirect competition among species. More phylogeny-based studies on connections between niche diversification and speciation are needed across many insect taxa, especially in groups that exhibit few host shifts in relation to speciation. C1 [Nyman, Tommi] Univ Eastern Finland, Dept Biol, FI-80101 Joensuu, Finland. [Smith, David R.] ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. [Boeve, Jean-Luc] Royal Belgian Inst Nat Sci, Dept Entomol, B-1000 Brussels, Belgium. RP Nyman, T (reprint author), Univ Eastern Finland, Dept Biol, POB 111, FI-80101 Joensuu, Finland. EM Tommi.Nyman@uef.fi FU European Community [BE-TAF-1462]; Academy of Finland [124695] FX We especially wish to thank colleagues who provided samples of higher-nematine species, many of which would otherwise have been impossible to obtain: Lauri Kapari, Heikki Roininen, Alexey Zinovjev, Ewald Altenhofer, Mikk Heidemaa, Marko Prous, Akira Yamagami, Matti Viitasaari, Herbert R. Jacobson, Valerie Caron, Urs Schaffner, Jens Rydell, Jeffrey Joy, and B. DeJonge. We also thank two anonymous referees for their constructive criticisms, which helped to improve the manuscript. The Centre of Scientific Computing in Helsinki and the Cyberinfrastructure for Phylogenetic Research (CIPRES) project in San Diego allocated computing resources for phylogenetic analyses on their servers. This research was initiated with support from the SYNTHESYS Project http://www.synthesys.info which is financed by the European Community Research Infrastructure Action under the FP6 "Structuring the European Research Area Programme" (project BE-TAF-1462), and the main part of the funding was provided by the Academy of Finland (project 124695 for TN). NR 95 TC 46 Z9 47 U1 2 U2 42 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2148 J9 BMC EVOL BIOL JI BMC Evol. Biol. PD SEP 1 PY 2010 VL 10 AR 266 DI 10.1186/1471-2148-10-266 PG 13 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 661YI UT WOS:000282768900001 PM 20807452 ER PT J AU Saarela, JM Peterson, PM Elizondo, MSG Rosen, DJ AF Saarela, Jeffery M. Peterson, Paul M. Gonzalez Elizondo, M. Socorro Rosen, David J. TI Eleocharis cryptica (Cyperaceae), a dwarf new species from Durango, Mexico SO BRITTONIA LA English DT Article DE conservation; Eleocharis nigrescens; Sierra Madre Occidental; Tenuissimae ID INFRAGENERIC CLASSIFICATION; LIMNOCHLOA CYPERACEAE; NOMENCLATURE; TAXONOMY; FLORA AB Eleocharis cryptica (Cyperaceae), known from pine-oak forest in Durango, Mexico, is described and illustrated. It belongs to Eleocharis subg. Eleocharis ser. Tenuissimae and can be distinguished by its diminutive size, with culms 2-13 mm long (including spikelets 1.3-1.7 mm long), and the folliform prolongations of its upper sheaths. It is the smallest species of Eleocharis thus far known. C1 [Saarela, Jeffery M.] Canadian Museum Nat, Ottawa, ON K1P 6P4, Canada. [Peterson, Paul M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Gonzalez Elizondo, M. Socorro] IPN, CIIDIR, Unidad Durango, Durango 34220, Mexico. [Rosen, David J.] Texas A&M Univ, Dept Ecosyst Sci & Management, SM Tracy Herbarium, College Stn, TX 77843 USA. RP Saarela, JM (reprint author), Canadian Museum Nat, POB 3443,Stn D, Ottawa, ON K1P 6P4, Canada. EM jsaarela@mus-nature.ca FU Smithsonian Institutions Restricted Endowment fund; National Geographic Society Committee for Research and Exploration [8087-06]; Canadian Museum of Nature FX We thank Christopher S. Reid for field assistance, Julian Starr for helpful discussion, Alice Tangerini for preparing the illustration, and the constructive comments of two reviewers. Our field research was supported financially by the Smithsonian Institutions Restricted Endowment fund, the National Geographic Society Committee for Research and Exploration (grant number 8087-06) and the Canadian Museum of Nature. NR 47 TC 4 Z9 5 U1 0 U2 1 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0007-196X J9 BRITTONIA JI Brittonia PD SEP PY 2010 VL 62 IS 3 BP 233 EP 238 DI 10.1007/s12228-009-9111-y PG 6 WC Plant Sciences SC Plant Sciences GA 651BY UT WOS:000281900800007 ER PT J AU Stellaccio, AE AF Stellaccio, Anthony E. TI Asuurkeraamika SO CERAMICS-ART AND PERCEPTION LA English DT Article C1 [Stellaccio, Anthony E.] Smithsonian Inst, Natl Museum African Art, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU CERAMICS-ART & PERCEPTION PTY LTD PI SHERIDAN PA 23 N SCOTT ST, STE 16, SHERIDAN, WYOMING 82801 USA SN 1035-1841 J9 CERAMICS-ART PERCEPT JI Ceramics-Art Percept. PD SEP-NOV PY 2010 IS 81 BP 48 EP 51 PG 4 WC Art SC Art GA 643XQ UT WOS:000281334400012 ER PT J AU Liebherr, JK Casale, A Erwin, TL Ball, GE AF Liebherr, James K. Casale, Achille Erwin, Terry L. Ball, George E. TI ON THE PROVENANCE OF BOHEMAN'S "EUGENIES RESA" CARABIDAE (COLEOPTERA) ALLEGEDLY DESCRIBED FROM HAWAII SO COLEOPTERISTS BULLETIN LA English DT Article DE ground beetles; taxonomy; biogeography; distribution; new synonymies AB Five carabid beetle species described from the Hawaiian Islands, Polynesia-Calleida gracilis Gemminger and de Harold, 1868 (= Calleida amoenula Boheman, 1858), Calleida sanguinicollis Dejean, 1831 (= Calleida insularis Boheman, 1858), Lebia insularis Boheman, 1858, Selenophorus insularis Boheman, 1858, and Selenophorus picinus Boheman, 1858 are shown to be properly attributed to the American biogeographic region, with their type localities corrected to either Central America or Pacific South America. Two of the five names are newly synonymized: L. insularis Boheman = L. analis Dejean, 1825 (new synonymy), and S. insularis Boheman = S. chalcosomus Reiche, 1843 (new synonymy), Calleida gracilis is shown to be a member taxon of the janthina species-group of South America, most similar to Calleida tibialis Brulle, 1837. However, taxonomic uncertainty surrounding C. gracilis, C. tibialis, and an undescribed taxon precludes definitive species circumscription in this group, and C. gracilis is retained as a valid member of the janthina species-group pending future revision. Selenophorus picinus is placed as species incertae sedis within Selenophorus subgenus Gynandropus Dejean, alternately treated as the hylacis species-group. The biogeographical and ecological consequences obtained from removing these taxa from the Polynesian fauna include: 1) recognition of more natural biogeographical distributions for the genera Calleida Latreille and Dejean, Lebia Latreille, and Selenophorus Dejean; 2) elimination of all examples that could demonstrate extinction of a non-native carabid beetle species subsequent to its accidental introduction into the Hawaiian Islands. C1 [Liebherr, James K.] Cornell Univ, Dept Entomol, Ithaca, NY 14853 USA. [Casale, Achille] Univ Sassari, Dipartimento Zool & Genet Evoluzionist, I-07100 Sassari, Italy. [Erwin, Terry L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Ball, George E.] Univ Alberta, Dept Biol Sci, Edmonton, AB T6G 2E3, Canada. RP Liebherr, JK (reprint author), Cornell Univ, Dept Entomol, Ithaca, NY 14853 USA. EM jkl5@cornell.edu; casale@uniss.it; erwint@si.edu; gball@ualberta.ca NR 38 TC 0 Z9 0 U1 1 U2 2 PU COLEOPTERISTS SOC PI ATHENS PA UNIV GEORGIA, 413 BIOLOGICAL SCIENCES BUILDING, ATHENS, GA 30602-2603 USA SN 0010-065X J9 COLEOPTS BULL JI Coleopt. Bull. PD SEP PY 2010 VL 64 IS 3 BP 221 EP 229 PG 9 WC Entomology SC Entomology GA 658XZ UT WOS:000282530000007 ER PT J AU Aiello, A Nunez, ED Stockwell, HP AF Aiello, Annette Dominguez Nunez, Edwin Stockwell, Henry P. TI NOTHING IS PERFECT: BIODEGRADABLE PACKING MATERIAL AS FOOD AND TRANSPORTATION FOR A MUSEUM PEST, LASIODERMA SERRICORNE (F.) (COLEOPTERA: ANOBIIDAE) SO COLEOPTERISTS BULLETIN LA English DT Editorial Material C1 [Aiello, Annette; Dominguez Nunez, Edwin; Stockwell, Henry P.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Aiello, A (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. NR 5 TC 0 Z9 1 U1 3 U2 11 PU COLEOPTERISTS SOC PI ATHENS PA UNIV GEORGIA, 413 BIOLOGICAL SCIENCES BUILDING, ATHENS, GA 30602-2603 USA SN 0010-065X J9 COLEOPTS BULL JI Coleopt. Bull. PD SEP PY 2010 VL 64 IS 3 BP 256 EP 257 PG 2 WC Entomology SC Entomology GA 658XZ UT WOS:000282530000012 ER PT J AU Cusatti, UV Garay, AL Johnson, PJ AF Vargas Cusatti, Ursula Lanuza Garay, Alfredo Johnson, Paul J. TI NEW RECORDS OF PLATYCREPIDIUS COSTARICENSIS JOHNSON AND PLATYCREPIDIUS EBURATUS (CHAMPION) (COLEOPTERA: ELATERIDAE) IN PANAMA SO COLEOPTERISTS BULLETIN LA English DT Editorial Material C1 [Vargas Cusatti, Ursula] Univ Panama, Colon, Panama. [Lanuza Garay, Alfredo] Smithsonian Trop Res Inst, Punta Galeta Marine Lab, Colon, Panama. [Johnson, Paul J.] S Dakota State Univ, Brookings, SD 57007 USA. RP Cusatti, UV (reprint author), Univ Panama, Colon, Panama. EM ucusatti@hotmail.com; lanuzaa@si.edu; paul.johnson@sdstate.edu NR 6 TC 1 Z9 1 U1 0 U2 0 PU COLEOPTERISTS SOC PI ATHENS PA UNIV GEORGIA, 413 BIOLOGICAL SCIENCES BUILDING, ATHENS, GA 30602-2603 USA SN 0010-065X J9 COLEOPTS BULL JI Coleopt. Bull. PD SEP PY 2010 VL 64 IS 3 BP 285 EP 286 PG 2 WC Entomology SC Entomology GA 658XZ UT WOS:000282530000018 ER PT J AU Clark, MA Babich, R Barros, K Brower, RC Rebbi, C AF Clark, M. A. Babich, R. Barros, K. Brower, R. C. Rebbi, C. TI Solving lattice QCD systems of equations using mixed precision solvers on GPUs SO COMPUTER PHYSICS COMMUNICATIONS LA English DT Article DE CUDA; GPGPU; CPU; Lattice QCD; Mixed precision AB Modern graphics hardware is designed for highly parallel numerical tasks and promises significant cost and performance benefits for many scientific applications. One such application is lattice quantum chromodynamics (lattice QCD), where the main computational challenge is to efficiently solve the discretizecl Dirac equation in the presence of an SU(3) gauge field. Using NVIDIA's CUDA platform we have implemented a Wilson-Dirac sparse matrix-vector product that performs at up to 40, 135 and 212 Gflops for double, single and half precision respectively on NVIDIA's GeForce GTX 280 CPU. We have developed a new mixed precision approach for Krylov solvers using reliable updates which allows for full double precision accuracy while using only single or half precision arithmetic for the bulk of the computation. The resulting BiCGstab and CG solvers run in excess of 100 Gflops and, in terms of iterations until convergence, perform better than the usual defect-correction approach for mixed precision. (C) 2010 Elsevier B.V. All rights reserved. C1 [Clark, M. A.] Harvard Univ, Sch Engn & Appl Sci, Initiat Innovat Comp, Cambridge, MA 02138 USA. [Clark, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Babich, R.; Brower, R. C.; Rebbi, C.] Boston Univ, Ctr Computat Sci, Boston, MA 02215 USA. [Babich, R.; Brower, R. C.; Rebbi, C.] Boston Univ, Dept Phys, Boston, MA 02215 USA. [Barros, K.] Northwestern Univ, Dept Engn Sci & Appl Math, Evanston, IL 60208 USA. [Barros, K.] Northwestern Univ, Dept Mat Sci & Engn, Evanston, IL 60208 USA. RP Clark, MA (reprint author), Harvard Univ, Sch Engn & Appl Sci, Initiat Innovat Comp, 29 Oxford St, Cambridge, MA 02138 USA. EM mikec@seas.harvard.edu FU US DOE [DE-FG02-91ER40676, DE-FC02-06ER41440]; NSF [DGE-0221680, PHY-0427646, PHY-0835713, OCI-0749300] FX This work was supported in part by US DOE grants DE-FG02-91ER40676 and DE-FC02-06ER41440 and NSF grants DGE-0221680, PHY-0427646, PHY-0835713 and OCI-0749300. We would like to thank D. Luebke of NVIDIA for generous hardware donations and G. Shi for improving the numerical stability of the half precision 8 parameter reconstruction. NR 20 TC 85 Z9 85 U1 0 U2 12 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0010-4655 J9 COMPUT PHYS COMMUN JI Comput. Phys. Commun. PD SEP PY 2010 VL 181 IS 9 BP 1517 EP 1528 DI 10.1016/j.cpc.2010.05.002 PG 12 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA 638DX UT WOS:000280873500005 ER PT J AU Newsome, SD Bentall, GB Tinker, MT Oftedal, OT Ralls, K Estes, JA Fogel, ML AF Newsome, Seth D. Bentall, Gena B. Tinker, M. Tim Oftedal, Olav T. Ralls, Katherine Estes, James A. Fogel, Marilyn L. TI Variation in delta C-13 and delta N-15 diet-vibrissae trophic discrimination factors in a wild population of California sea otters SO ECOLOGICAL APPLICATIONS LA English DT Article DE Enhydra lutris nereis; San Nicolas Island, California, USA; sea otter; stable isotopes; trophic discrimination factors (TDFs); vibrissae ID ISOTOPE MIXING MODELS; FOOD WEB STRUCTURE; STABLE-ISOTOPES; NUTRITIONAL STRESS; NITROGEN-BALANCE; FORAGING ECOLOGY; CARBON ISOTOPES; AMINO-ACIDS; ENRICHMENT; FRACTIONATION AB The ability to quantify dietary inputs using stable isotope data depends on accurate estimates of isotopic differences between a consumer (c) and its diet (d), commonly referred to as trophic discrimination factors (TDFs) and denoted by Delta(c-d). At present, TDFs are available for only a few mammals and are usually derived in captive settings. The magnitude of TDFs and the degree to which they vary in wild populations is unknown. We determined delta C-13 and delta N-15 TDFs for vibrissae (i.e., whiskers), a tissue that is rapidly becoming an informative isotopic substrate for ecologists, of a wild population of sea otters for which individual diet has been quantified through extensive observational study. This is one of the very few studies that report TDFs for free-living wild animals feeding on natural diets. Trophic discrimination factors of 2.2 parts per thousand +/- 0.7 parts per thousand for delta C-13 and 3.5 parts per thousand +/- 0.6 parts per thousand for delta N-15 (mean +/- SD) were similar to those reported for captive carnivores, and variation in individual delta C-13 TDFs was negatively but significantly related to sea urchin consumption. This pattern may relate to the lipid-rich diet consumed by most sea otters in this population and suggests that it may not be appropriate to lipid-extract prey samples when using the isotopic composition of keratinaceous tissues to examine diet in consumers that frequently consume lipid-rich foods, such as many marine mammals and seabirds. We suggest that inherent variation in TDFs should be included in isotopically based estimates of trophic level, food chain length, and mixing models used to quantify dietary inputs in wild populations; this practice will further define the capabilities and limitations of isotopic approaches in ecological studies. C1 [Newsome, Seth D.; Fogel, Marilyn L.] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. [Bentall, Gena B.] Monterey Bay Aquarium, Sea Otter Res & Conservat, Monterey, CA 93940 USA. [Tinker, M. Tim; Estes, James A.] Univ Calif Santa Cruz, Ctr Ocean Hlth, Long Marine Lab, Santa Cruz, CA 95060 USA. [Oftedal, Olav T.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Ralls, Katherine] Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. RP Newsome, SD (reprint author), Univ Wyoming, Dept Zool & Physiol, 1000 E Univ Ave,Dept 3166, Laramie, WY 82071 USA. EM snewsome@uwyo.edu RI Tinker, Martin/F-1277-2011 FU Monterey Bay National Marine Sanctuary Foundation; U.S. Marine Mammal Commission; National Science Foundation [ATM-0502491]; Carnegie Institution of Washington; W. M. Keck Foundation [072000] FX Thanks to the Monterey Bay National Marine Sanctuary Foundation and the U.S. Marine Mammal Commission for funding the collection and processing of prey samples. We thank E. Snyder, C. Mancuso, W. Wurzel, E. Heil, and R. Harley for laboratory assistance; A. Green, M. Kenner, K. Miles, and J. Bodkin for assistance in prey collection; and K. Fox-Dobbs, D. H. Monson, A. C. Jakle, B. Fry, and C. Martinez del Rio for constructive reviews. We thank A. Green for obtaining the necessary California Fish and Game permit for marine invertebrate collection and the U. S. Navy for permission to conduct research on San Nicolas Island. S. D. Newsome was partially funded by the National Science Foundation (ATM-0502491), Carnegie Institution of Washington, and the W. M. Keck Foundation (072000). NR 42 TC 50 Z9 50 U1 8 U2 43 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1051-0761 J9 ECOL APPL JI Ecol. Appl. PD SEP PY 2010 VL 20 IS 6 BP 1744 EP 1752 DI 10.1890/09-1502.1 PG 9 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 643EN UT WOS:000281278500020 PM 20945772 ER PT J AU Mangan, SA Herre, EA Bever, JD AF Mangan, Scott A. Herre, Edward A. Bever, James D. TI Specificity between Neotropical tree seedlings and their fungal mutualists leads to plant-soil feedback SO ECOLOGY LA English DT Article DE arbuscular mycorrhizal fungi (AMF); Barro Colorado Island, Panama; belowground interactions; Glomus spp.; light level; plant-fungal interactions; plant-soil feedback; specificity; tropical forest ID ARBUSCULAR MYCORRHIZAL FUNGI; TROPICAL FOREST; NEGATIVE FEEDBACK; SPATIAL-PATTERNS; COMMUNITY STRUCTURE; MAINTAIN DIVERSITY; LIGHT-INTENSITY; GROWTH; PATHOGENS; COLONIZATION AB A growing body of evidence obtained largely from temperate grassland studies suggests that feedbacks occurring between plants and their associated soil biota are important to plant community assemblage. However, few studies have examined the importance of soil organisms in driving plant-soil feedbacks in forested systems. In a tropical forest in central Panama, we examined whether interactions between tree seedlings and their associated arbuscular mycorrhizal fungi (AMF) lead to plant-soil feedback. Specifically, do tropical seedlings modify their own AMF communities in a manner that either favors or inhibits the next cohort of conspecific seedlings (i.e., positive or negative feedback, respectively)? Seedlings of two shade-tolerant tree species (Eugenia nesiotica, Virola surinamensis) and two pioneer tree species (Luehea seemannii, Apeiba aspera) were grown in pots containing identical AMF communities composed of equal amounts of inoculum of six co-occurring AMF species. The different AMF-host combinations were all exposed to two light levels. Under low light (2% PAR), only two of the six AMF species sporulated, and we found that host identity did not influence composition of AMF spore communities. However, relative abundances of three of the four AMF species that produced spores were influenced by host identity when grown under high light (20% PAR). Furthermore, spores of one of the AMF species, Glomus geosporum, were common in soils of Luehea and Eugenia but absent in soils of Apeiba and Virola. We then conducted a reciprocal experiment to test whether AMF communities previously modified by Luehea and Apeiba differentially affected the growth of conspecific and heterospecific seedlings. Luehea seedling growth did not differ between soils containing AMF communities modified by Luehea and Apeiba. However, Apeiba seedlings were significantly larger when grown with Apeiba-modified AMF communities, as compared to Apeiba seedlings grown with Luehea-modifed AMF communities. Our experiments suggest that interactions between tropical trees and their associated AMF are species-specific and that these interactions may shape both tree and AMF communities through plant-soil feedback. C1 [Mangan, Scott A.; Bever, James D.] Indiana Univ, Dept Biol, Bloomington, IN 47405 USA. [Mangan, Scott A.; Herre, Edward A.] Smithsonian Trop Res Inst, Dpo, AA 34002 USA. RP Mangan, SA (reprint author), Indiana Univ, Dept Biol, Bloomington, IN 47405 USA. EM smangan37@gmail.com FU Smithsonian Tropical Research Institute (STRI); National Science Foundation [DIGG-0308779, DEB-0049080, DEB-0616891]; Indiana University; American Mammalogy Society; Sigma Xi FX We are indebted to Dora Alvarez, Camila Pizano, Charlotte Jander, Andrea Vincent, and Robert Horan for their assistance. We thank two anonymous reviewers for improving this manuscript. This work would not have been possible without the logistical support and funding provided by the Smithsonian Tropical Research Institute (STRI predoctoral fellowship to S. A. Mangan and a soil initiative grant to E. A. Herre). The National Science Foundation provided grant DIGG-0308779 to S. A. Mangan and James D. Bever, and grants DEB-0049080 and DEB-0616891 to James D. Bever. Funding was also provided by Indiana University, Sigma Xi, and the American Mammalogy Society to S. A. Mangan. NR 45 TC 27 Z9 32 U1 5 U2 100 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 J9 ECOLOGY JI Ecology PD SEP PY 2010 VL 91 IS 9 BP 2594 EP 2603 DI 10.1890/09-0396.1 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 648MO UT WOS:000281698400016 PM 20957954 ER PT J AU Poorter, L Kitajima, K Mercado, P Chubina, J Melgar, I Prins, HHT AF Poorter, Lourens Kitajima, Kaoru Mercado, Pablo Chubina, Jose Melgar, Israel Prins, Herbert H. T. TI Resprouting as a persistence strategy of tropical forest trees: relations with carbohydrate storage and shade tolerance SO ECOLOGY LA English DT Article DE Bolivia; disturbance; dry forest; growth-survival trade-off; leaf size; resprouting; shade tolerance; total nonstructural carbohydrates (NSC); tropical rain forest; wood density ID LIFE-HISTORY VARIATION; RAIN-FOREST; DRY FOREST; INTERSPECIFIC VARIATION; LIGHT REQUIREMENTS; FUNCTIONAL TRAITS; SEEDLING SURVIVAL; LEAF TRAITS; GROWTH; ALLOCATION AB Resprouting is an important persistence strategy for woody species and represents a dominant pathway of regeneration in many plant communities, with potentially large consequences for vegetation dynamics, community composition, and species coexistence. Most of our knowledge of resprouting strategies comes from fire-prone systems, but this cannot be readily applied to other systems where disturbances are less intense. In this study we evaluated sapling responses to stem snapping for 49 moist-forest species and 36 dry-forest species from two Bolivian tropical forests. To this end we compared in a field experiment the survival and height growth of clipped and control saplings for a two-year period, and related this to the shade tolerance, carbohydrate reserves, and the morphological traits (wood density, leaf size) of the species. Nearly all saplings resprouted readily after stem damage, although dry-forest species realized, on average, a better survival and growth after stem damage compared to moist-forest species. Shade-tolerant species were better at resprouting than light-demanding species in moist forest. This resprouting ability is an important prerequisite for successful regeneration in the shaded understory, where saplings frequently suffer damage from falling debris. Survival after stem damage was, surprisingly, only modestly related to stem reserves, and much more strongly related to wood density, possibly because a high wood density enables plants to resist fungi and pathogens and to reduce stem decay. Correlations between sapling performance and functional traits were similar for the two forest types, and for phylogenetically independent contrasts and for cross-species analyses. The consistency of these results suggests that tropical forest species face similar trade-offs in different sites and converge on similar sets of solutions. A high resprouting ability, as well as investments in stem defense and storage reserves, form part of a suite of co-evolved traits that underlies the growth-survival trade-off, and contributes to light gradient partitioning and species coexistence. These links with shade tolerance are important in the moist evergreen forest, which casts a deep, more persistent shade, but tend to diminish in dry deciduous forest where light is a less limiting resource. C1 [Poorter, Lourens] Wageningen Univ, Ctr Ecosyst Studies, Forest Ecol & Forest Management Grp, NL-6700 AA Wageningen, Netherlands. [Poorter, Lourens; Mercado, Pablo; Chubina, Jose; Melgar, Israel] IBIF, Santa Cruz, Bolivia. [Poorter, Lourens; Prins, Herbert H. T.] Wageningen Univ, Ctr Ecosyst Studies, Resource Ecol Grp, NL-6700 AA Wageningen, Netherlands. [Kitajima,